WorldWideScience

Sample records for charged scalar field

  1. Gravitational collapse of charged scalar fields

    CERN Document Server

    Torres, Jose M

    2014-01-01

    In order to study the gravitational collapse of charged matter we analyze the simple model of an self-gravitating massless scalar field coupled to the electromagnetic field in spherical symmetry. The evolution equations for the Maxwell-Klein-Gordon sector are derived in the 3+1 formalism, and coupled to gravity by means of the stress-energy tensor of these fields. To solve consistently the full system we employ a generalized Baumgarte-Shapiro-Shibata-Nakamura (BSSN) formulation of General Relativity that is adapted to spherical symmetry. We consider two sets of initial data that represent a time symmetric spherical thick shell of charged scalar field, and differ by the fact that one set has zero global electrical charge while the other has non-zero global charge. For compact enough initial shells we find that the configuration doesn't disperse and approaches a final state corresponding to a sub-extremal Reissner-N\\"ordstrom black hole with $|Q|charge of the scalar field $...

  2. Charged Scalars in Transient Stellar Electromagnetic Fields

    Institute of Scientific and Technical Information of China (English)

    Marina-Aura Dariescu; Ciprian Dariescu; Ovidiu Buhucianu

    2011-01-01

    We consider a non-rotating strongly magnetized object, whose magnetic induction isof the form Bx = Bo{t)sin kz. In the electromagnetic field generated by only one component of the four-vector potential, we solve the Klein-Gordon equation and discuss the sudden growth of the scalar wave functions for wavenumbers inside computable ranges. In the case of unexcited transversal kinetic degrees, we write down the recurrent differential system for the amplitude functions and compute the respective conserved currents.

  3. Effect of scalar field mass on gravitating charged scalar solitons and black holes in a cavity

    CERN Document Server

    Ponglertsakul, Supakchai

    2016-01-01

    We study soliton and black hole solutions of Einstein charged scalar field theory in cavity. We examine the effect of introducing a scalar field mass on static, spherically symmetric solutions of the field equations. We focus particularly on the spaces of soliton and black hole solutions, as well as studying their stability under linear, spherically symmetric perturbations of the metric, electromagnetic field, and scalar field.

  4. Study of symmetry breaking of charged scalar field: Hydrodynamic version

    CERN Document Server

    Matos, T

    2015-01-01

    We rewrite the Klein-Gordon (KG) equation for a complex scalar field as a new Gross-Pitaevskii (GP)-like equation. The potential of the scalar field is a mexican-hat potential and the field is in a thermal bath with one loop contribution. We interpret the new GP equation as a finite temperature generalization of the GP equation for a charged field. We find its hydrodynamic version as well and using it, we derive the corresponding thermodynamics. We also obtain a generalized first law for a charged Bose-Einstein Condensate (BEC).

  5. Study of symmetry breaking of charged scalar field: Hydrodynamic version

    Science.gov (United States)

    Matos, T.; Rodríguez-Meza, M. A.

    2014-11-01

    We rewrite the Klein-Gordon (KG) equation for a complex scalar field as a new Gross-Pitaevskii (GP)-like equation. The potential of the scalar field is a mexican-hat potential and the field is in a thermal bath with one loop contribution. We interpret the new GP equation as a finite temperature generalization of the GP equation for a charged field. We find its hydrodynamic version as well and using it, we derive the corresponding thermodynamics. We also obtain a generalized first law for a charged Bose-Einstein Condensate (BEC).

  6. Black hole solutions in Einstein-charged scalar field theory

    OpenAIRE

    Ponglertsakul, S.; Dolan, S.; Winstanley, E.

    2015-01-01

    We investigate possible end-points of the superradiant instability for a charged black hole with a reflecting mirror. By considering a fully coupled system of gravity and a charged scalar field, hairy black hole solutions are obtained. The linear stability of these black hole solutions is studied.

  7. Phantom collapse of electrically charged scalar field in dilaton gravity

    CERN Document Server

    Nakonieczna, Anna

    2013-01-01

    Our research focus on gravitational collapse of electrically charged scalar field in dilaton gravity and in the presence of phantom coupling. We examine dynamical behaviour of the scalar field coupled to Maxwell field when gravitational interactions have form consistent with the low-energy limit of the string theory. Moreover, we allow the evolving fields to have negative sign in front of the respective kinetic term of the Lagrangian. The main aim of our studies is to investigate in what manner does the phantom nature of either Maxwell or dilaton fields (or both of them) affect the outcomes of the collapse. It turns out that the influence is crucial to the obtained spacetime structures. Negative kinetic energy of one (or both) of the fields delays, changes the course or even prevents the collapse.

  8. Conserved Charges of Minimal Massive Gravity Coupled to Scalar Field

    CERN Document Server

    Setare, M R

    2016-01-01

    Recently, the theory of Topologically massive gravity non-minimally coupled to a scalar field has been proposed which comes from Lorentz-Chern-Simons theory \\cite{1}. That theory is a torsion free one. We extend that theory by adding an extra term which makes torsion to be non-zero. The extended theory can be regarded as an extension of Minimal massive gravity such that it is non-minimally coupled to a scalar field. We obtain equations of motion of extended theory such that they are expressed in terms of usual torsion free spin-connection. We show that BTZ spacetime is a solution of this theory when scalar field is constant. We define quasi-local conserved charge by the concept of generalized off-shell ADT current which both are conserved for any asymptotically Killing vector field as well as a Killing vector field which is admitted by spacetime everywhere. Also we find general formula for entropy of stationary black hole solution in the context of considered theory. We apply the obtained formulas on BTZ blac...

  9. Superradiant instability of charged scalar field in stringy black hole mirror system

    Energy Technology Data Exchange (ETDEWEB)

    Li, Ran; Zhao, Junkun [Henan Normal University, Department of Physics, Xinxiang (China)

    2014-09-15

    It has been shown that the mass of a charged scalar field in the background of a charged stringy black hole is never able to generate a potential well outside the event horizon to trap the superradiant modes. This is to say that the charged stringy black hole is stable against massive charged scalar perturbations. In this paper we will study the superradiant instability of the massless scalar field in the background of charged stringy black hole due to a mirror-like boundary condition. The analytical expression of the frequencies of unstable superradiant modes is derived by using the asymptotic matching method. It is also pointed out that the black hole mirror system becomes extremely unstable for a large charge q of the scalar field and a small mirror radius r{sub m}. (orig.)

  10. No-go theorem for static scalar field dark matter halos with no Noether charges

    Science.gov (United States)

    Diez-Tejedor, Alberto; Gonzalez-Morales, Alma X.

    2013-09-01

    Classical scalar fields have been considered as a possible effective description of dark matter. We show that, for any metric theory of gravity, no static, spherically symmetric, regular, spatially localized, attractive, stable spacetime configuration can be sourced by the coherent excitation of a scalar field with positive definite energy density and no Noether charges. In the weak field regime, the result also applies for configurations with a repulsive gravitational potential. This extends Derrick’s theorem to the case of a general (noncanonical) scalar field, including the self-gravitational effects. Some possible ways out are briefly discussed.

  11. A no-go result for static scalar field dark matter halos with no Noether charges

    CERN Document Server

    Diez-Tejedor, Alberto

    2013-01-01

    Classical scalar fields have been proposed as a possible solution to the dark matter problem in galaxies. We show that, within the framework of general relativity, no static, spherically symmetric, regular, spatially localized, attractive, stable configuration can be sourced by the coherent excitation of a scalar field with positive definite energy density and no Noether charges. This result extends Derrick's theorem to the case of a general (non-canonical) scalar field, including the self-gravitational effects. Some possible way-outs are briefly discussed.

  12. Dark sector impact on gravitational collapse of an electrically charged scalar field

    Science.gov (United States)

    Nakonieczna, Anna; Rogatko, Marek; Nakonieczny, Łukasz

    2015-11-01

    Dark matter and dark energy are dominating components of the Universe. Their presence affects the course and results of processes, which are driven by the gravitational interaction. The objective of the paper was to examine the influence of the dark sector on the gravitational collapse of an electrically charged scalar field. A phantom scalar field was used as a model of dark energy in the system. Dark matter was modeled by a complex scalar field with a quartic potential, charged under a U(1)-gauge field. The dark components were coupled to the electrically charged scalar field via the exponential coupling and the gauge field-Maxwell field kinetic mixing, respectively. Complete non-linear simulations of the investigated process were performed. They were conducted from regular initial data to the end state, which was the matter dispersal or a singularity formation in a spacetime. During the collapse in the presence of dark energy dynamical wormholes and naked singularities were formed in emerging spacetimes. The wormhole throats were stabilized by the violation of the null energy condition, which occurred due to a significant increase of a value of the phantom scalar field function in its vicinity. The square of mass parameter of the dark matter scalar field potential controlled the formation of a Cauchy horizon or wormhole throats in the spacetime. The joint impact of dark energy and dark matter on the examined process indicated that the former decides what type of an object forms, while the latter controls the amount of time needed for the object to form. Additionally, the dark sector suppresses the natural tendency of an electrically charged scalar field to form a dynamical Reissner-Nordström spacetime during the gravitational collapse.

  13. Infrared Behaviour of Landau Gauge Yang-Mills Theory with a Fundamentally Charged Scalar Field

    CERN Document Server

    Fister, Leonard

    2010-01-01

    The infrared behaviour of the n-point functions of a Yang-Mills theory with a charged scalar field in the fundamental representation of SU(N) is studied in the formalism of Dyson-Schwinger equations. Assuming a stable skeleton expansion solutions in form of power laws for the Green functions are obtained. For a massless scalar field the uniform limit is sufficient to describe the infrared scaling behaviour of vertices. Not taking into account a possible Higgs-phase it turns out that kinematic singularities play an important role for the scaling solutions of massive scalars. On a qualitative level scalar Yang-Mills theory yields similar scaling solutions as recently obtained for QCD.

  14. Dark sector impact on gravitational collapse of an electrically charged scalar field

    CERN Document Server

    Nakonieczna, Anna; Nakonieczny, Łukasz

    2015-01-01

    Dark matter and dark energy are dominating components of the Universe. Their presence affects the course and results of processes, which are driven by the gravitational interaction. The objective of the paper was to examine the influence of the dark sector on the gravitational collapse of an electrically charged scalar field. A phantom scalar field was used as a model of dark energy in the system. Dark matter was modeled by a complex scalar field with a quartic potential, charged under an U(1)-gauge field. The dark components were coupled to the electrically charged scalar field via the exponential coupling and the gauge field-Maxwell field kinetic mixing, respectively. Complete non-linear simulations of the investigated process were performed. They were conducted from regular initial data to the end state, which was the matter dispersal or a singularity formation in a spacetime. During the collapse in the presence of dark energy dynamical wormholes and naked singularities were formed in emerging spacetimes. ...

  15. Superradiance of a charged scalar field coupled to the Einstein-Maxwell equations

    CERN Document Server

    Baake, Olaf

    2016-01-01

    We consider the Einstein-Maxwell-Klein-Gordon equations for a spherically symmetric scalar field scattering off a Reissner-Nordstr\\"om black hole in asymptotically flat spacetime. The equations are solved numerically using a hyperboloidal evolution scheme. For suitable frequencies of the initial data, superradiance is observed, leading to a substantial decrease of mass and charge of the black hole. We also derive a Bondi mass loss formula using the Kodama vector field and investigate the late-time decay of the scalar field.

  16. Finite temperature Casimir effect for charged massless scalars in a magnetic field

    CERN Document Server

    Erdas, Andrea

    2013-01-01

    The zeta function regularization technique is used to study the finite temperature Casimir effect for a charged and massless scalar field confined between parallel plates and satisfying Dirichlet boundary conditions at the plates. A magnetic field perpendicular to the plates is included. Three equivalent expressions for the zeta function are obtained, which are exact to all orders in the magnetic field strength, temperature and plate distance. These expressions of the zeta function are used to calculate the Helmholtz free energy of the scalar field and the pressure on the plates, in the case of high temperature, small plate distance and strong magnetic field. In all cases, simple analytic expressions are obtained for the free energy and pressure which are accurate and valid for practically all values of temperature, plate distance and magnetic field.

  17. The charged black-hole bomb: A lower bound on the charge-to-mass ratio of the explosive scalar field

    OpenAIRE

    Hod, Shahar

    2016-01-01

    The well-known superradiant amplification mechanism allows a charged scalar field of proper mass $\\mu$ and electric charge $q$ to extract the Coulomb energy of a charged Reissner-Nordstr\\"om black hole. The rate of energy extraction can grow exponentially in time if the system is placed inside a reflecting cavity which prevents the charged scalar field from escaping to infinity. This composed black-hole-charged-scalar-field-mirror system is known as the {\\it charged black-hole bomb}. Previous...

  18. Analytic treatment of the system of a Kerr-Newman black hole and a charged massive scalar field

    Science.gov (United States)

    Hod, Shahar

    2016-08-01

    Charged rotating Kerr-Newman black holes are known to be superradiantly unstable to perturbations of charged massive bosonic fields whose proper frequencies lie in the bounded regime 0 velocity and electric potential of the Kerr-Newman black hole, and {m ,q ,μ } are, respectively, the azimuthal harmonic index, the charge-coupling constant, and the proper mass of the field. In this paper we study analytically the complex resonance spectrum which characterizes the dynamics of linearized charged massive scalar fields in a near-extremal Kerr-Newman black hole spacetime. Interestingly, it is shown that near the critical frequency ωc for superradiant amplification and in the eikonal large-mass regime, the superradiant instability growth rates of the explosive scalar fields are characterized by a nontrivial (nonmonotonic) dependence on the dimensionless charge-to-mass ratio q /μ . In particular, for given parameters {M ,Q ,J } of the central Kerr-Newman black hole, we determine analytically the optimal charge-to-mass ratio q /μ of the explosive scalar field which maximizes the growth rate of the superradiant instabilities in the composed Kerr-Newman-black-hole-charged-massive-scalar-field system.

  19. The charged black-hole bomb: A lower bound on the charge-to-mass ratio of the explosive scalar field

    Directory of Open Access Journals (Sweden)

    Shahar Hod

    2016-04-01

    Full Text Available The well-known superradiant amplification mechanism allows a charged scalar field of proper mass μ and electric charge q to extract the Coulomb energy of a charged Reissner–Nordström black hole. The rate of energy extraction can grow exponentially in time if the system is placed inside a reflecting cavity which prevents the charged scalar field from escaping to infinity. This composed black-hole-charged-scalar-field-mirror system is known as the charged black-hole bomb. Previous numerical studies of this composed physical system have shown that, in the linearized regime, the inequality q/μ>1 provides a necessary condition for the development of the superradiant instability. In the present paper we use analytical techniques to study the instability properties of the charged black-hole bomb in the regime of linearized scalar fields. In particular, we prove that the lower bound qμ>rm/r−−1rm/r+−1 provides a necessary condition for the development of the superradiant instability in this composed physical system (here r± are the horizon radii of the charged Reissner–Nordström black hole and rm is the radius of the confining mirror. This analytically derived lower bound on the superradiant instability regime of the composed black-hole-charged-scalar-field-mirror system is shown to agree with direct numerical computations of the instability spectrum.

  20. Vacuum pair production of charged scalar bosons in time-dependent electric fields

    CERN Document Server

    Li, Zi-Liang; Xie, Bai-Song

    2013-01-01

    Based on the quantum mechanical scattering model, the dynamical assist effect and the multiple-slit interference effect in electron-positron pair production from vacuum are generalized to vacuum pair production of charged scalar bosons. For the former effect some combinations of a strong but slowly varying electric field and a weak but rapidly varying one with different time delay are studied. Results indicate that the oscillation intensity of momentum spectrum and the number density of created bosons reduce with increasing of the time delay. Obviously, they achieve the maximum if the time delay equals zero. For the latter effect, it is shown that this effect does not exist for equal-sign $N$-pulse electric field in contrast to its existence for alternating-sign $N$-pulse. An approximate solution of boson momentum spectrum is got and it is agreeable well with the exact numerical one in alternating-sign $N$-pulse electric field, especially for $2$-pulse field and for small longitudinal momentum. The difference...

  1. Slowly decaying resonances of charged massive scalar fields in the Reissner-Nordström black-hole spacetime

    Science.gov (United States)

    Hod, Shahar

    2016-10-01

    We determine the characteristic timescales associated with the linearized relaxation dynamics of the composed Reissner-Nordström-black-hole-charged-massive-scalar-field system. To that end, the quasinormal resonant frequencies {ωn(μ , q , M , Q) }n = 0 n = ∞ which characterize the dynamics of a charged scalar field of mass μ and charge coupling constant q in the charged Reissner-Nordström black-hole spacetime of mass M and electric charge Q are determined analytically in the eikonal regime 1 ≪ Mμ black-hole electric charge Q / M, the imaginary part of the resonant oscillation frequency is a monotonically decreasing function of the dimensionless ratio μ / q. In particular, it is shown that the quasinormal resonance spectrum is characterized by the asymptotic behavior ℑ ω → 0 in the limiting case Mμ → qQ. This intriguing finding implies that the composed Reissner-Nordström-black-hole-charged-massive-scalar-field system is characterized by extremely long relaxation times τrelax ≡ 1 / ℑ ω → ∞ in the Mμ / qQ →1- limit.

  2. Slowly decaying resonances of charged massive scalar fields in the Reissner–Nordström black-hole spacetime

    Directory of Open Access Journals (Sweden)

    Shahar Hod

    2016-10-01

    Full Text Available We determine the characteristic timescales associated with the linearized relaxation dynamics of the composed Reissner–Nordström-black-hole-charged-massive-scalar-field system. To that end, the quasinormal resonant frequencies {ωn(μ,q,M,Q}n=0n=∞ which characterize the dynamics of a charged scalar field of mass μ and charge coupling constant q in the charged Reissner–Nordström black-hole spacetime of mass M and electric charge Q are determined analytically in the eikonal regime 1≪Mμcharge Q/M, the imaginary part of the resonant oscillation frequency is a monotonically decreasing function of the dimensionless ratio μ/q. In particular, it is shown that the quasinormal resonance spectrum is characterized by the asymptotic behavior ℑω→0 in the limiting case Mμ→qQ. This intriguing finding implies that the composed Reissner–Nordström-black-hole-charged-massive-scalar-field system is characterized by extremely long relaxation times τrelax≡1/ℑω→∞ in the Mμ/qQ→1− limit.

  3. The charged black-hole bomb: A lower bound on the charge-to-mass ratio of the explosive scalar field

    CERN Document Server

    Hod, Shahar

    2016-01-01

    The well-known superradiant amplification mechanism allows a charged scalar field of proper mass $\\mu$ and electric charge $q$ to extract the Coulomb energy of a charged Reissner-Nordstr\\"om black hole. The rate of energy extraction can grow exponentially in time if the system is placed inside a reflecting cavity which prevents the charged scalar field from escaping to infinity. This composed black-hole-charged-scalar-field-mirror system is known as the {\\it charged black-hole bomb}. Previous numerical studies of this composed physical system have shown that, in the linearized regime, the inequality $q/\\mu>1$ provides a necessary condition for the development of the superradiant instability. In the present paper we use analytical techniques to study the instability properties of the charged black-hole bomb in the regime of linearized scalar fields. In particular, we prove that the lower bound ${{q}\\over{\\mu}}>\\sqrt{{{r_{\\text{m}}/r_--1}\\over{r_{\\text{m}}/r_+-1}}}$ provides a necessary condition for the develo...

  4. Hawking Radiation from Spherically Symmetrical Gravitational Collapse to an Extremal R-N Black Hole for a Charged Scalar Field

    Institute of Scientific and Technical Information of China (English)

    ZHANG Hong-Bao; CAO Zhou-Jian; GAO Chong-Shou

    2004-01-01

    Si-Jie Gao has recently investigated Hawking radiation from spherically symmetrical gravitational collapse to an extremal R-N black hole for a real scalar field. Especially he estimated the upper bound for the expected number of particles in any wave packet belonging to Hout spontaneously produced from the state |0>in, which confirms the traditional belief that extremal black holes do not radiate particles. Making some modifications, we demonstrate that the analysis can go through for a charged scalar field.

  5. On the evolution equations for a self-gravitating charged scalar field

    CERN Document Server

    Pugliese, Daniela

    2013-01-01

    We consider a complex scalar field minimally coupled to gravity and to a U(1) gauge symmetry and we construct of a first order symmetric hyperbolic evolution system for the Einstein-Maxwell-Klein-Gordon system. Our analysis is based on a 1+3 tetrad formalism which makes use of the components of the Weyl tensor as one of the unknowns. In order to ensure the symmetric hyperbolicity of the evolution equations, implied by the Bianchi identity, we introduce a tensor of rank 3 corresponding to the covariant derivative of the Faraday tensor, and two tensors of rank 2 for the covariant derivative of the vector potential and the scalar field.

  6. Structure Scalars In Charged Plane Symmetry

    CERN Document Server

    Sharif, M

    2013-01-01

    We consider non-adiabatic flow of the fluid possessing dissipation in the form of shearing viscosity in electromagnetic field. The scalar functions (structure scalars) for charged plane symmetry are formulated and are related with the physical variables of the fluid. We also develop a relationship between the Weyl tensor and other physical variables by using Taub mass formalism. The role of electric charge as well as its physical significance for the evolution of the shear tensor and expansion scalar are also explored. Finally, we discuss a special case for dust with cosmological constant.

  7. Slowly decaying resonances of charged massive scalar fields in the Reissner-Nordstr\\"om black-hole spacetime

    CERN Document Server

    Hod, Shahar

    2016-01-01

    We determine the characteristic timescales associated with the linearized relaxation dynamics of the composed Reissner-Nordstr\\"om-black-hole-charged-massive-scalar-field system. To that end, the quasinormal resonant frequencies $\\{\\omega_n(\\mu,q,M,Q)\\}_{n=0}^{n=\\infty}$ which characterize the dynamics of a charged scalar field of mass $\\mu$ and charge coupling constant $q$ in the charged Reissner-Nordstr\\"om black-hole spacetime of mass $M$ and electric charge $Q$ are determined {\\it analytically} in the eikonal regime $1\\ll M\\mucharge $Q/M$, the imaginary part of the resonant oscillation frequency is a monotonically {\\it decreasing} function of the dimensionless ratio $\\mu/q$. In particular, it is shown that the quasinormal resonance spectrum is characterized by the asymptotic behavior $\\Im\\omega\\to0$ in the limiting case $M\\mu\\to qQ$. This intriguing finding implies that the composed Reissner-Nordstr\\"om-black-...

  8. Stationary Charged Scalar Clouds around Black Holes in String Theory

    CERN Document Server

    Bernard, Canisius

    2016-01-01

    It was reported that Kerr-Newman black holes can support linear charged scalar field in their exterior regions. This stationary massive charged scalar field can form a bound-state and these bound-states are called stationary scalar clouds. In this paper, we study that Kerr-Sen black holes can also support stationary massive charged scalar clouds by matching the near and far region solutions of the radial part of Klein-Gordon wave equation. We also review stationary scalar clouds within the background of static electrically charged black hole solution in the low energy limit of heterotic string field theory namely the GMGHS black holes.

  9. Analytic treatment of the system of a Kerr-Newman black hole and a charged massive scalar field

    CERN Document Server

    Hod, Shahar

    2016-01-01

    Charged rotating Kerr-Newman black holes are known to be superradiantly unstable to perturbations of charged massive bosonic fields whose proper frequencies lie in the bounded regime $0 < \\omega < \\text{min} \\{\\omega_{\\text{c}} \\equiv m \\Omega_{\\text{H}} + q\\Phi_{\\text{H}},\\mu\\}$ [here $\\{\\Omega_{\\text{H}}, \\Phi_{\\text{H}}\\}$ are respectively the angular velocity and electric potential of the Kerr-Newman black hole, and $\\{m,q,\\mu\\}$ are respectively the azimuthal harmonic index, the charge coupling constant, and the proper mass of the field]. In this paper we study analytically the complex resonance spectrum which characterizes the dynamics of linearized charged massive scalar fields in a near-extremal Kerr-Newman black-hole spacetime. Interestingly, it is shown that near the critical frequency $\\omega_{\\text{c}}$ for superradiant amplification and in the eikonal large-mass regime, the superradiant instability growth rates of the explosive scalar fields are characterized by a non-trivial (non-monotonic...

  10. How many scalar fields there are and how are they related to fermions and weak bosons in the spin-charge-family theory?

    CERN Document Server

    Borstnik, Norma Susana Mankoc

    2012-01-01

    The spin-charge-family theory offers a possible explanation for the assumptions of the standard model, interpreting the standard model as its low energy effective manifestation. The standard model Higgs and Yukawa couplings are explained as an effective replacement for several scalar fields, all of bosonic (adjoint) representations with respect to all the charge groups, with the family groups included. Assuming the Lagrange function for all scalar fields to be of the renormalizable kind, properties of the scalar fields on the tree level are discussed. Free scalar fields (mass eigenstates) differ from either those, which couple to $Z_m$, or to $W^{\\pm}_{m}$ or to each family member of each of the four families, which further differ among themselves. Consequently the spin-charge-family theory predictions differ from those of the standard model.

  11. The spin-charge-family theory explains why are the scalar fields (the Higgs) doublets with respect to the weak and the hyper charge

    CERN Document Server

    Borstnik, Norma Susana Mankoc

    2014-01-01

    One Weyl representation of SO(13+1) contains, if analysed with respect to the charge and the spin groups of the standard model, left handed weak (SU(2)_{I}) charged and SU(2)_{II} chargeless colour triplet quarks and colourless leptons, and right handed weakless and SU(2)_{II} charged quarks and leptons (neutrinos and electrons). In the spin-charge-family theory spinors carry also the family quantum numbers, explaining the origin of families and correspondingly the masses of fermions and weak bosons and the origin of the scalar Higgs and Yukawa couplings. It is demonstrated in this paper that all the fields appearing in the simple starting action of spin-charge-family theory in d=(13+1) with the scalar index with respect to d=(3+1) and determining masses of quarks and leptons (and correspondingly also of the weak boson fields) carry the weak and the hyper charge in the fundamental representations, in agreement with the Higgs in the standard model.

  12. Universality in the relaxation dynamics of the composed black-hole-charged-massive-scalar-field system: The role of quantum Schwinger discharge

    Directory of Open Access Journals (Sweden)

    Shahar Hod

    2015-07-01

    Full Text Available The quasinormal resonance spectrum {ωn(μ,q,M,Q}n=0n=∞ of charged massive scalar fields in the charged Reissner–Nordström black-hole spacetime is studied analytically in the large-coupling regime qQ≫Mμ (here {μ,q} are respectively the mass and charge coupling constant of the field, and {M,Q} are respectively the mass and electric charge of the black hole. This physical system provides a striking illustration for the validity of the universal relaxation bound τ×T≥ħ/π in black-hole physics (here τ≡1/ℑω0 is the characteristic relaxation time of the composed black-hole-scalar-field system, and T is the Bekenstein–Hawking temperature of the black hole. In particular, it is shown that the relaxation dynamics of charged massive scalar fields in the charged Reissner–Nordström black-hole spacetime may saturate this quantum time-times-temperature inequality. Interestingly, we prove that potential violations of the bound by light scalar fields are excluded by the Schwinger-type pair-production mechanism (a vacuum polarization effect, a quantum phenomenon which restricts the physical parameters of the composed black-hole-charged-field system to the regime qQ≪M2μ2/ħ.

  13. Quantum radiation from an inertial scalar charge evolving in the de Sitter universe: Weak-field limit

    Energy Technology Data Exchange (ETDEWEB)

    Blaga, Robert, E-mail: robert.blaga90@e-uvt.ro [Faculty of Physics, West University of Timişoara V. Pârvan Ave. 4, RO-300223 Timişoara (Romania)

    2015-12-07

    We investigate the energy radiated by an inertial scalar charge evolving in the expanding Poincaré patch of de Sitter spacetime, in the framework of scalar QED perturbation theory. We approximate the transition amplitude in the small expansion parameter limit and show that the leading contribution to the radiated energy has the form of the energy radiated by an accelerated particle in Minkowski space.

  14. Conformal scalar field wormholes

    Science.gov (United States)

    Halliwell, Jonathan J.; Laflamme, Raymond

    1989-01-01

    The Euclidian Einstein equations with a cosmological constant and a conformally coupled scalar field are solved, taking the metric to be of the Robertson-Walker type. In the case Lambda = 0, solutions are found which represent a wormhole connecting two asymptotically flat Euclidian regions. In the case Lambda greater than 0, the solutions represent tunneling from a small Tolman-like universe to a large Robertson-Walker universe.

  15. Structure Scalars for Charged Cylindrically Symmetric Relativistic Fluids

    CERN Document Server

    Sharif, M

    2012-01-01

    We investigate some structure scalars developed through Riemann tensor for self-gravitating cylindrically symmetric charged dissipative anisotropic fluid. We show that these scalars are directly related to the fundamental properties of the fluid. We formulate dynamical-transport equation as well as the mass function by including charge which are then expressed in terms of structure scalars. The effects of electric charge are investigated in the structure and evolution of compact objects. Finally, we show that all possible solutions of the field equations can be written in terms of these scalars.

  16. Stability of gravitating charged-scalar solitons in a cavity

    CERN Document Server

    Ponglertsakul, Supakchai; Dolan, Sam R

    2016-01-01

    We present new regular solutions of Einstein-charged scalar field theory in a cavity. The system is enclosed inside a reflecting mirror-like boundary, on which the scalar field vanishes. The mirror is placed at the zero of the scalar field closest to the origin, and inside this boundary our solutions are regular. We study the stability of these solitons under linear, spherically symmetric perturbations of the metric, scalar and electromagnetic fields. If the radius of the mirror is sufficiently large, we present numerical evidence for the stability of the solitons. For small mirror radius, some of the solitons are unstable. We discuss the physical interpretation of this instability.

  17. Scalar clouds in charged stringy black hole-mirror system

    Energy Technology Data Exchange (ETDEWEB)

    Li, Ran; Zhao, Junkun; Wu, Xinghua; Zhang, Yanming [Henan Normal University, Department of Physics, Xinxiang (China)

    2015-04-15

    It was reported that massive scalar fields can form bound states around Kerr black holes (Herdeiro and Radu, Phys. Rev. Lett. 112:221101, 2014). These bound states are called scalar clouds; they have a real frequency ω = mΩ{sub H}, where m is the azimuthal index and Ω{sub H} is the horizon angular velocity of Kerr black hole. In this paper, we study scalar clouds in a spherically symmetric background, i.e. charged stringy black holes, with the mirror-like boundary condition. These bound states satisfy the superradiant critical frequency condition ω = qΦ{sub H} for a charged scalar field, where q is the charge of the scalar field, and Φ{sub H} is the horizon's electrostatic potential. We show that, for the specific set of black hole and scalar field parameters, the clouds are only possible for specific mirror locations r{sub m}. It is shown that analytical results of the mirror location r{sub m} for the clouds perfectly coincide with numerical results in the qQ << 1 regime. We also show that the scalar clouds are also possible when the mirror locations are close to the horizon. Finally, we provide an analytical calculation of the specific mirror locations rm for the scalar clouds in the qQ >> 1 regime. (orig.)

  18. Ultrarelativistic boost with scalar field

    Science.gov (United States)

    Svítek, O.; Tahamtan, T.

    2016-02-01

    We present the ultrarelativistic boost of the general global monopole solution which is parametrized by mass and deficit solid angle. The problem is addressed from two different perspectives. In the first one the primary object for performing the boost is the metric tensor while in the second one the energy momentum tensor is used. Since the solution is sourced by a triplet of scalar fields that effectively vanish in the boosting limit we investigate the behavior of a scalar field in a simpler setup. Namely, we perform the boosting study of the spherically symmetric solution with a free scalar field given by Janis, Newman and Winicour. The scalar field is again vanishing in the limit pointing to a broader pattern of scalar field behaviour during an ultrarelativistic boost in highly symmetric situations.

  19. Symmetry inheritance of scalar fields

    Science.gov (United States)

    Smolić, Ivica

    2015-07-01

    Matter fields do not necessarily have to share the symmetries with the spacetime they live in. When this happens, we speak of the symmetry inheritance of fields. In this paper we classify the obstructions of symmetry inheritance by the scalar fields, both real and complex, and look more closely at the special cases of stationary and axially symmetric spacetimes. Since the symmetry noninheritance is present in the scalar fields of boson stars and may enable the existence of the black hole scalar hair, our results narrow the possible classes of such solutions. Finally, we define and analyse the symmetry noninheritance contributions to the Komar mass and angular momentum of the black hole scalar hair.

  20. Symmetry inheritance of scalar fields

    CERN Document Server

    Smolić, Ivica

    2015-01-01

    Matter fields don't necessarily have to share the symmetries with the spacetime they live in. When this happens, we speak of the symmetry inheritance of fields. In this paper we classify the obstructions of symmetry inheritance by the scalar fields, both real and complex, and look more closely at the special cases of stationary and axially symmetric spacetimes. Since the symmetry noninheritance is present in the scalar fields of boson stars and may enable the existence of the black hole scalar hair, our results narrow the possible classes of such solutions. Finally, we define and analyse the symmetry noninheritance contributions to Komar mass and angular momentum of the black hole scalar hair.

  1. Spherically symmetric scalar field collapse

    Indian Academy of Sciences (India)

    Koyel Ganguly; Narayan Banerjee

    2013-03-01

    It is shown that a scalar field, minimally coupled to gravity, may have collapsing modes even when the energy condition is violated, that is, for ( + 3) < 0. This result may be useful in the investigation of the possible clustering of dark energy. All the examples dealt with have apparent horizons formed before the formation of singularity. The singularities formed are shell focussing in nature. The density of the scalar field distribution is seen to diverge at singularity. The Ricci scalar also diverges at the singularity. The interior spherically symmetric metric is matched with exterior Vaidya metric at the hypersurface and the appropriate junction conditions are obtained.

  2. Electrically charged Kerr black holes with scalar hair

    CERN Document Server

    Delgado, Jorge F M; Radu, Eugen; Runarsson, Helgi

    2016-01-01

    We construct electrically charged Kerr black holes (BHs) with scalar hair. Firstly, we take an uncharged scalar field, interacting with the electromagnetic field only indirectly, via the background metric. The corresponding family of solutions, dubbed Kerr-Newman BHs with ungauged scalar hair, reduces to (a sub-family of) Kerr-Newman BHs in the limit of vanishing scalar hair and to uncharged rotating boson stars in the limit of vanishing horizon. It adds one extra parameter to the uncharged solutions: the total electric charge. This leading electromagnetic multipole moment is unaffected by the scalar hair and can be computed by using Gauss's law on any closed 2-surface surrounding (a spatial section of) the event horizon. By contrast, the first sub-leading electromagnetic multipole -- the magnetic dipole moment --, gets suppressed by the scalar hair, such that the gyromagnetic ratio is always smaller than the Kerr-Newman value ($g=2$). Secondly, we consider a gauged scalar field and obtain a family of Kerr-Ne...

  3. Particles and scalar waves in noncommutative charged black hole spacetime

    OpenAIRE

    Bhar, Piyali; Rahaman, Farook; Biswas, Ritabrata(Indian Institute of Engineering Sceince and Technology Shibpur (Formerly, Bengal Engineering and Science University Shibpur), 711 013, Howrah, West Bengal, India); Mondal, U. F.

    2015-01-01

    In this paper we have discussed geodesics and the motion of test particle in the gravitational field of noncommutative charged black hole spacetime. The motion of massive and massless particle have been discussed seperately. A comparative study of noncommutative charged black hole and usual Reissner-Nordstrom black hole has been done. The study of effective potential has also been included. Finally, we have examined the scattering of scalar waves in noncommutative charged black hole spacetime.

  4. Particles and Scalar Waves in Noncommutative Charged Black Hole Spacetime

    Science.gov (United States)

    Piyali, Bhar; Farook, Rahaman; Ritabrata, Biswas; U. F., Mondal

    2015-07-01

    In this paper we have discussed geodesics and the motion of test particle in the gravitational field of non-commutative charged black hole spacetime. The motion of massive and massless particle have been discussed seperately. A comparative study of noncommutative charged black hole and usual Reissner-Nordström black hole has been done. The study of effective potential has also been included. Finally, we have examined the scattering of scalar waves in noncommutative charged black hole spacetime.

  5. Stationary scalar configurations around extremal charged black holes

    CERN Document Server

    Degollado, Juan Carlos

    2013-01-01

    We consider the minimally coupled Klein-Gordon equation for a charged, massive scalar field in the non-extremal Reissner-Nordstr\\"om background. Performing a frequency domain analysis, using a continued fraction method, we compute the frequencies \\omega for quasi-bound states. We observe that, as the extremal limit for both the background and the field is approached, the real part of the quasi-bound states frequencies $\\mathcal{R}(\\omega)$ tends to the mass of the field and the imaginary part $\\mathcal{I}(\\omega)$ tends to zero, for any angular momentum quantum number $\\ell$. The limiting frequencies in this double extremal limit are shown to correspond to a distribution of extremal scalar particles, at stationary positions, in no-force equilibrium configurations with the background. Thus, generically, these stationary scalar configurations are regular at the event horizon. If, on the other hand, the distribution contains scalar particles at the horizon, the configuration becomes irregular therein, in agreeme...

  6. Electromagnetic Form Factor of Charged Scalar Meson

    Institute of Scientific and Technical Information of China (English)

    LI Heng-Mei; CHEN Ning; WANG Zhi-Gang; WAN Shao-Long

    2007-01-01

    Wavefunctions and the electromagnetic form factor of charged scalar mesons are studied with the vector-vectortype flat-bottom potential model under the framework of the spinor spinor Bethe Salpeter equation. The obtained results are in agreement with other theories.

  7. Properties of twice four families of quarks and leptons, of scalars and gauge fields as predicted by the spin-charge-family theory

    CERN Document Server

    Borstnik, Norma Susana Mankoc

    2013-01-01

    The spin-charge-family theory, proposed by the author as a possible new way to explain the assumptions of the standard model, predicts at the low energy regime two decoupled groups of four families of quarks and leptons. In two successive breaks the massless families, first the group of four and at the second break the rest four families, gain nonzero mass matrices. The families are identical with respect to the charges and spin. There are two kinds of fields in this theory, which manifest at low energies as the gauge vector and scalar fields: the fields which couple to the charges and spin, and the fields which couple to the family quantum numbers. In loop corrections to the tree level mass matrices both kinds start to contribute coherently. The fourth family of the lower group of four families is predicted to be possibly observed at the LHC and the stable of the higher four families -- the fifth family -- is the candidate to constitute the dark matter. Properties of the families of quarks and leptons and of...

  8. The traversable wormhole with classical scalar fields

    OpenAIRE

    Kim, S. -W; Kim, S. P.

    1999-01-01

    We study the Lorentzian static traversable wormholes coupled to quadratic scalar fields. We also obtain the solutions of the scalar fields and matters in the wormhole background and find that the minimal size of the wormhole should be quantized under the appropriate boundary conditions for the positive non-minimal massive scalar field.

  9. Scalar Fields in Particle Physics

    CERN Document Server

    Pedro, Leonardo

    2016-01-01

    Extending the scalar sector helps in studying the Higgs mechanism and some Standard Model problems. We implement the correspondence between the gauge-dependent elementary states and the non-perturbative non-abelian gauge-invariant asymptotic states, necessary to study the non-perturbative phenomenology of two-Higgs-doublet models. The Flavour and CP violation in experimental data follows a hierarchical pattern, accounted by the Standard Model. We define the Minimal Flavour Violation condition with six spurions in effective field theories, implying Flavour and CP violation entirely dependent on the fermion mixing matrices but independent of the fermion masses hierarchy; it is renormalization-group invariant. We study the phenomenology of renormalizable two-Higgs-doublet models which verify the defined condition as consequence of a symmetry; new light physical scalars, mediating Flavour Changing Neutral Currents, are allowed by flavour data without flavour coefficients beyond the Standard Model; we tested the m...

  10. Entropic quantization of scalar fields

    Energy Technology Data Exchange (ETDEWEB)

    Ipek, Selman; Caticha, Ariel [Department of Physics, University at Albany-SUNY, Albany, NY 12222 (United States)

    2015-01-13

    Entropic Dynamics is an information-based framework that seeks to derive the laws of physics as an application of the methods of entropic inference. The dynamics is derived by maximizing an entropy subject to constraints that represent the physically relevant information that the motion is continuous and non-dissipative. Here we focus on the quantum theory of scalar fields. We provide an entropic derivation of Hamiltonian dynamics and using concepts from information geometry derive the standard quantum field theory in the Schrödinger representation.

  11. Entropic quantization of scalar fields

    Science.gov (United States)

    Ipek, Selman; Caticha, Ariel

    2015-01-01

    Entropic Dynamics is an information-based framework that seeks to derive the laws of physics as an application of the methods of entropic inference. The dynamics is derived by maximizing an entropy subject to constraints that represent the physically relevant information that the motion is continuous and non-dissipative. Here we focus on the quantum theory of scalar fields. We provide an entropic derivation of Hamiltonian dynamics and using concepts from information geometry derive the standard quantum field theory in the Schrödinger representation.

  12. Renormalizability and the Scalar Field

    CERN Document Server

    Sastry, R R

    1999-01-01

    The infinite dimensional generalization of the quantum mechanics of extended objects, namely, the quantum field theory of extended objects is presented. The paradigm example studied in this paper is the Euclidean scalar field with a found to be finite when the virtual particle intermediate states are characterized by fuzzy particles instead of ordinary pointlike particles. Causality, Lorentz invariance, and unitarity (verified up to fourth order in the coupling constant) are preserved in the theory. In addition, the Kallen-Lehmann spectral representation for the propagator is discussed.

  13. Gravitational Frames and Scalar Field Dynamics

    CERN Document Server

    Ozaydin, M T

    2016-01-01

    Scalar fields describe interesting phenomena such as Higgs bosons, dark matter and dark energy, and are found to be quite common in physical theories. These fields are susceptible to gravitational forces so that being massless is not enough to remain conformal invariant. They should also be connected directly to the scalar curvature. Because of this characteristics, we investigated the structure and interactions of scalar fields under the conformal transformations. We show how to reduce the quadratic quantum contributions in the single scalar field theory. In the multi-scalar field theories, we analyzed interactions in certain limits. We suggest a new method for stabilizing Higgs bosons.

  14. Vacuum expectation values of the current density and energy-momentum tensor for a charged scalar field in curved spacetime with toroidally compactified spatial dimensions

    Science.gov (United States)

    Saharian, Aram; Kotanjyan, Anna; Sargsyan, Hayk; Simonyan, David

    2016-07-01

    The models with compact spatial dimensions appear in a number of fundamental physical theories. In particular, the idea of compactified dimensions has been extensively used in supergravity and superstring theories. In quantum field theory, the modification of the vacuum fluctuations spectrum by the periodicity conditions imposed on the field operator along compact dimensions leads to a number of interesting physical effects. A well known example of this kind, demonstrating the close relation between quantum phenomena and global geometry, is the topological Casimir effect. In models with extra compact dimensions, the Casimir energy creates a nontrivial potential for the compactification radius. This can serve as a stabilization mechanism for moduli fields and for the effective gauge couplings. The Casimir effect has also been considered as a possible origin for the dark energy in Kaluza-Klein-type and braneworld models. In the resent presentation we investigate the effects of the gravity and topology on the local properties of the quantum vacuum for a charged scalar field in the presence of a classical gauge field. Vacuum expectation value of the energy-momentum tensor and current density are investigated for a charged scalar field in dS spacetime with toroidally compact spatial dimensions in the presence of a classical constant gauge field. Due to the nontrivial topology, the latter gives rise to Aharonov-Bohm-like effect on the vacuum characteristics. The vacuum current density, energy density and stresses are even periodic functions of the magnetic flux enclosed by compact dimensions. For small values of the comoving lengths of compact dimensions, compared with the dS curvature radius, the effects of gravity on the topological contributions are small and the expectation values are expressed in terms of the corresponding quantities in the Minkowski bulk by the standard conformal relation. For large values of the comoving lengths, depending on the field mass, two

  15. Scalar Field (Wave) Dark Matter

    CERN Document Server

    Matos, T

    2016-01-01

    Recent high-quality observations of dwarf and low surface brightness (LSB) galaxies have shown that their dark matter (DM) halos prefer flat central density profiles. On the other hand the standard cold dark matter model simulations predict a more cuspy behavior. Feedback from star formation has been widely used to reconcile simulations with observations, this might be successful in field dwarf galaxies but its success in low mass galaxies remains uncertain. One model that have received much attention is the scalar field dark matter model. Here the dark matter is a self-interacting ultra light scalar field that forms a cosmological Bose-Einstein condensate, a mass of $10^{-22}$eV/c$^2$ is consistent with flat density profiles in the centers of dwarf spheroidal galaxies, reduces the abundance of small halos, might account for the rotation curves even to large radii in spiral galaxies and has an early galaxy formation. The next generation of telescopes will provide better constraints to the model that will help...

  16. Discrete Scalar Quantum Field Theory

    CERN Document Server

    Gudder, Stan

    2016-01-01

    We begin with a description of spacetime by a 4-dimensional cubic lattice $\\sscript$. It follows from this framework that the the speed of light is the only nonzero instantaneous speed for a particle. The dual space $\\sscripthat$ corresponds to a cubic lattice of energy-momentum. This description implies that there is a discrete set of possible particle masses. We then define discrete scalar quantum fields on $\\sscript$. These fields are employed to define interaction Hamiltonians and scattering operators. Although the scattering operator $S$ cannot be computed exactly, approximations are possible. Whether $S$ is unitary is an unsolved problem. Besides the definitions of these operators, our main assumption is conservation of energy-momentum for a scattering process. This article concludes with various examples of perturbation approximations. These include simplified versions of electron-electron and electron-proton scattering as well as simple decay processes. We also define scattering cross-sections, decay ...

  17. Bulk scalar field in DGP braneworld cosmology

    CERN Document Server

    Ansari, Rizwan ul Haq

    2007-01-01

    We investigated the effects of bulk scalar field in the braneworld cosmological scenario. The Friedmann equations and acceleration condition in presence of the bulk scalar field for a zero tension brane and cosmological constant are studied. In DGP model the effective Einstein equation on the brane is obtained with bulk scalar field. The rescaled bulk scalar field on the brane in the DGP model behaves as an effective four dimensional field, thus standard type cosmology is recovered. In present study of the DGP model, the late-time accelerating phase of the universe can be explained .

  18. Gravitational Frames and Scalar Field Dynamics

    OpenAIRE

    Ozaydin, M. T.; Pirinccioglu, N.

    2016-01-01

    Scalar fields describe interesting phenomena such as Higgs bosons, dark matter and dark energy, and are found to be quite common in physical theories. These fields are susceptible to gravitational forces so that being massless is not enough to remain conformal invariant. They should also be connected directly to the scalar curvature. Because of this characteristics, we investigated the structure and interactions of scalar fields under the conformal transformations. We show how to reduce the q...

  19. Unified Dark Matter Scalar Field Models

    Directory of Open Access Journals (Sweden)

    Daniele Bertacca

    2010-01-01

    of a single scalar field accounts for a unified description of the Dark Matter and Dark Energy sectors, dubbed Unified Dark Matter (UDM models. In this framework, we consider the general Lagrangian of -essence, which allows to find solutions around which the scalar field describes the desired mixture of Dark Matter and Dark Energy. We also discuss static and spherically symmetric solutions of Einstein's equations for a scalar field with noncanonical kinetic term, in connection with galactic halo rotation curves.

  20. Late-Time Evolution of Charged Gravitational Collapse and Decay of Charged Scalar Hair, 2

    CERN Document Server

    Hod, S; Hod, Shahar; Piran, Tsvi

    1998-01-01

    We study analytically the initial value problem for a charged massless scalar-field on a Reissner-Nordström spacetime. Using the technique of spectral decomposition we extend recent results on this problem. Following the no-hair theorem we reveal the dynamical physical mechanism by which the charged hair is radiated away. We show that the charged perturbations decay according to an inverse power-law behaviour at future timelike infinity and along future null infinity. Along the future outer horizon we find an oscillatory inverse power-law relaxation of the charged fields. We find that a charged black hole becomes ``bald'' slower than a neutral one, due to the existence of charged perturbations. Our results are also important to the study of mass-inflation and the stability of Cauchy horizons during a dynamical gravitational collapse of charged matter in which a charged black-hole is formed.

  1. All static and electrically charged solutions with Einstein base manifold of Einstein-Maxwell massless scalar field system in arbitrary dimensions

    CERN Document Server

    Maeda, Hideki

    2016-01-01

    We present a simple and complete classification of static solutions in the Einstein-Maxwell system with a massless scalar field in arbitrary $n(\\ge 3)$ dimensions. We consider spacetimes which correspond to a warped product $M^2 \\times K^{n-2}$, where $K^{n-2}$ is a $(n-2)$-dimensional Einstein space. The scalar field is assumed to depend only on the radial coordinate and the electromagnetic field is purely electric. The general solution with a non-constant real scalar field consists of seven solutions for $n\\ge 4$ and three solutions for $n=3$. None of them is endowed of a Killing horizon in accordance with the no-hair theorem.

  2. New type scalar fields for cosmic acceleration

    Energy Technology Data Exchange (ETDEWEB)

    Kehagias, A; Pakis, S [Department of Physics, National Technical University of Athens, GR-15773, Zografou, Athens (Greece)

    2007-05-15

    We present a model where a non-conventional scalar field may act like dark energy and leads to cosmic acceleration. The latter is driven by an appropriate field configuration, which result in an effective cosmological constant. The potential role of such a scalar in the cosmological constant problem is also discussed.

  3. Scalar field mass in generalized gravity

    OpenAIRE

    Faraoni, Valerio

    2009-01-01

    The notions of mass and range of a Brans-Dicke-like scalar field in scalar-tensor and f(R) gravity are subject to an ambiguity that hides a potential trap. We spell out this ambiguity and identify a physically meaningful and practical definition for these quantities. This is relevant when giving a mass to this scalar in order to circumvent experimental limits on the PPN parameters coming from Solar System experiments.

  4. Multiple critical gravitational collapse of charged scalar with reflecting wall

    CERN Document Server

    Cai, Rong-Gen

    2016-01-01

    In this paper, we present the results on the gravitational collapse of charged massless scalar field in asymptotically flat spacetime with a perfectly reflecting wall. Differing from previous works, we study the system in the double null coordinates, by which we could simulate the system until the black hole forms with higher precision but less performance time. We investigate the influence of charge on the black hole formation and the scaling behavior near the critical collapses. The gapless and gapped critical behaviors for black hole mass and charge are studied numerically. We find that they satisfy the scaling laws for critical gravitational collapse but the gapped critical behavior is different from its AdS counterpart.

  5. Primordial fluctuations without scalar fields

    CERN Document Server

    Magueijo, J

    2009-01-01

    We revisit the question of whether fluctuations in hydrodynamical, adiabatical matter could explain the observed structures in our Universe. We consider matter with variable equation of state $w=p_0/\\ep_0$ and a concomitant (under the adiabatic assumption) density dependent speed of sound, $c_s$. We find a limited range of possibilities for a set up when modes start inside the Hubble radius, then leaving it and freezing out. For expanding Universes, power-law $w(\\ep_0)$ models are ruled out (except when $c_s^2\\propto w \\ll 1$, requiring post-stretching the seeded fluctuations); but sharper profiles in $c_s$ do solve the horizon problem. Among these, a phase transition in $c_s$ is notable for leading to scale-invariant fluctuations if the initial conditions are thermal. For contracting Universes all power-law $w(\\ep_0)$ solve the horizon problem, but only one leads to scale-invariance: $w\\propto \\ep_0^2$ and $c_s\\propto \\ep_0$. This model bypasses a number of problems with single scalar field cyclic models (fo...

  6. Scalar field radiation from dilatonic black holes

    Science.gov (United States)

    Gohar, H.; Saifullah, K.

    2012-12-01

    We study radiation of scalar particles from charged dilaton black holes. The Hamilton-Jacobi method has been used to work out the tunneling probability of outgoing particles from the event horizon of dilaton black holes. For this purpose we use WKB approximation to solve the charged Klein-Gordon equation. The procedure gives Hawking temperature for these black holes as well.

  7. Charged scalar perturbations around Garfinkle–Horowitz–Strominger black holes

    Directory of Open Access Journals (Sweden)

    Cheng-Yong Zhang

    2015-10-01

    Full Text Available We examine the stability of the Garfinkle–Horowitz–Strominger (GHS black hole under charged scalar perturbations. Employing the appropriate numerical methods, we show that the GHS black hole is always stable against charged scalar perturbations. This is different from the results obtained in the de Sitter and anti-de Sitter black holes. Furthermore, we argue that in the GHS black hole background there is no amplification of the incident charged scalar wave to cause the superradiance, so that the superradiant instability cannot exist in this spacetime.

  8. Static scalar field solutions in symmetric gravity

    Science.gov (United States)

    Hossenfelder, S.

    2016-09-01

    We study an extension of general relativity with a second metric and an exchange symmetry between the two metrics. Such an extension might help to address some of the outstanding problems with general relativity, for example the smallness of the cosmological constant. We here derive a family of exact solutions for this theory. In this two-parameter family of solutions the gravitational field is sourced by a time-independent massless scalar field. We find that the only limit in which the scalar field entirely vanishes is flat space. The regular Schwarzschild-solution is left with a scalar field hidden in the second metric’s sector.

  9. Anomalous coupling of scalars to gauge fields

    Energy Technology Data Exchange (ETDEWEB)

    Brax, Philippe [CEA, IPhT, CNRS, URA 2306, Gif-sur-Yvette (France). Inst. de Physique Theorique; Burrage, Clare [Geneve Univ. (Switzerland). Dept. de Physique Theorique; Deutsches Elektronen-Synchrotron (DESY), Hamburg (Germany); Davis, Anne-Christine [Centre for Mathematical Sciences, Cambridge (United Kingdom). Dept. of Applied Mathematics and Theoretical Physics; Seery, David [Sussex Univ., Brighton (United Kingdom). Dept. of Physics and Astronomy; Weltman, Amanda [Cape Town Univ., Rondebosch (South Africa). Astronomy, Cosmology and Gravity Centre

    2010-10-15

    We study the transformation properties of a scalar-tensor theory, coupled to fermions, under the Weyl rescaling associated with a transition from the Jordan to the Einstein frame. We give a simple derivation of the corresponding modification to the gauge couplings. After changing frames, this gives rise to a direct coupling between the scalar and the gauge fields. (orig.)

  10. Exotic Material as Interactions Between Scalar Fields

    Directory of Open Access Journals (Sweden)

    Robertson G. A.

    2006-04-01

    Full Text Available Many theoretical papers refer to the need to create exotic materials with average negative energies for the formation of space propulsion anomalies such as "wormholes" and "warp drives". However, little hope is given for the existence of such material to resolve its creation for such use. From the standpoint that non-minimally coupled scalar fields to gravity appear to be the current direction mathematically. It is proposed that exotic material is really scalar field interactions. Within this paper the Ginzburg-Landau (GL scalar fields associated with superconductor junctions isinvestigated as a source for negative vacuum energy fluctuations, which could be used to study the interactions among energyfluctuations, cosmological scalar (i.e., Higgs fields, and gravity.

  11. Stationary axisymmetric spacetimes with a conformally coupled scalar field

    CERN Document Server

    Astorino, Marco

    2014-01-01

    Solution generating techniques for general relativity with a conformally (and minimally) coupled scalar field are pushed forward to build a wide class of asymptotically flat, axisymmetric and stationary spacetimes continuously connected to Kerr. This family contains, amongst other things, rotating extensions of the BBMB black hole and also its angular and mass multipolar generalisations. Further addition of NUT charge is also discussed.

  12. Gravitational Gauge Interactions of Scalar Field

    Institute of Scientific and Technical Information of China (English)

    WUNing

    2003-01-01

    Quantum gauge theory of gravity is formulated based on gauge principle. Because the Lagrangian has strict local gravitational gauge symmetry, gravitational gauge theory is a perturbatively renormalizable quantum theory. Gravitational gauge interactions of scalar field are studied in this paper. In quantum gauge theory of gravity, scalar field minimal couples to gravitational field through gravitational gauge covariant derivative. Comparing the Lagrangian for scalar field in quantum gauge theory of gravity with the corresponding Lagrangian in quantum fields in curved space-time, the definition for metric in curved space-time in geometry picture of gravity can be obtained, which is expressed by gravitational gauge field. In classical level, the Lagrangian and Hamiltonian approaches are also discussed.

  13. Gravitational Field Shielding by Scalar Field and Type II Superconductors

    Directory of Open Access Journals (Sweden)

    Zhang B. J.

    2013-01-01

    Full Text Available The gravitational field shielding by scalar field and type II superconductors are theoret- ically investigated. In accord with the well-developed five-dimensional fully covariant Kaluza-Klein theory with a scalar field, which unifies the Einsteinian general relativity and Maxwellian electromagnetic theory, the scalar field cannot only polarize the space as shown previously, but also flatten the space as indicated recently. The polariza- tion of space decreases the electromagnetic field by increasing the equivalent vacuum permittivity constant, while the flattening of space decreases the gravitational field by decreasing the equivalent gravitational constant. In other words, the scalar field can be also employed to shield the gravitational field. A strong scalar field significantly shield the gravitational field by largely decreasing the equivalent gravitational constant. According to the theory of gravitational field shielding by scalar field, the weight loss experimentally detected for a sample near a rotating ceramic disk at very low tempera- ture can be explained as the shielding of the Earth gravitational field by the Ginzburg- Landau scalar field, which is produced by the type II superconductors. The significant shielding of gravitational field by scalar field produced by superconductors may lead to a new spaceflight technology in future.

  14. Chaotic instantons in scalar field theory

    CERN Document Server

    Addazi, Andrea

    2016-01-01

    We consider a new class of instantons in context of quantum field theory of a scalar field coupled with a chaotic background source field. We show how the instanton associated to the quantum tunneling from a metastable false to the true vacuum will be corrected by an exponential enhancement factor. Possible implications are discussed.

  15. Intermediate inflation driven by DBI scalar field

    Science.gov (United States)

    Nazavari, N.; Mohammadi, A.; Ossoulian, Z.; Saaidi, Kh.

    2016-06-01

    Picking out a DBI scalar field as inflation, the slow-rolling inflationary scenario is studied by attributing an exponential time function to scale factor, known as intermediate inflation. The perturbation parameters of the model are estimated numerically for two different cases, and the final result is compared with Planck data. The diagram of tensor-to-scalar ratio r versus scalar spectra index ns is illustrated, and it is found that they are within an acceptable range as suggested by Planck. In addition, the acquired values for amplitude of scalar perturbation reveal the ability of the model to depict a good picture of the Universe in one of its earliest stages. As a further argument, the non-Gaussianity is investigated, displaying that the model prediction stands in a 68% C.L. regime according to the latest Planck data.

  16. Gravitational waves from scalar field accretion

    OpenAIRE

    Núnez, Darío; Degollado, Juan Carlos; Moreno, Claudia

    2011-01-01

    Our aim in this work is to outline some physical consequences of the interaction between black holes and scalar field halos in terms of gravitational waves. In doing so, the black hole is taken as a static and spherically symmetric gravitational source, {\\it i. e.} the Schwarzschild black hole, and we work within the test field approximation, considering that the scalar field lives in the curved space-time outside the black hole. We focused on the emission of gravitational waves when the blac...

  17. Gravitational peculiarities of a scalar field

    International Nuclear Information System (INIS)

    The zero-adjoint of a time-static Ricci-flat solution to Einstein's field equations is investigated. It represents a spacetime curved solely by a massless scalar field. The cylindrical symmetry is assumed to permit both planar and non-planar geodetic motions. Unusual, velocity-dependent gravitational features are encountered from these geodesics. (Author)

  18. Exact solutions for the biadjoint scalar field

    CERN Document Server

    White, Chris D

    2016-01-01

    Biadjoint scalar theories are novel field theories that arise in the study of non-abelian gauge and gravity amplitudes. In this short paper, we present exact nonperturbative solutions of the field equations, and compare their properties with monopole-like solutions in non-abelian gauge theory. Our results may pave the way for nonperturbative studies of the double copy.

  19. D-BIonic Screening of Scalar Fields

    CERN Document Server

    Burrage, Clare

    2014-01-01

    We study a new screening mechanism which is present in Dirac-Born-Infeld (DBI)-like theories. A scalar field with a DBI-like Lagrangian is minimally coupled to matter. In the vicinity of sufficiently dense sources, non-linearities in the scalar dominate and result in an approximately constant acceleration on a test particle, thereby suppressing the scalar force relative to gravity. Unlike generic P(X) theories, screening happens within the regime of validity of the effective field theory, thanks to the DBI symmetry. This symmetry also allows the removal of a constant field gradient, like in galileons. Not surprisingly, perturbations around the spherically-symmetry background propagate superluminally, but we argue for a chronology protection analogous to galileons. We derive constraints on the theory parameters from tests of gravity and discuss various extensions.

  20. Energy conditions and classical scalar fields

    CERN Document Server

    Bellucci, S

    2002-01-01

    Attention has been recently called upon the fact that the weak and null energy conditions and the second law of thermodynamics are violated in wormhole solutions of Einstein's theory with classical, nonminimally coupled, scalar fields as material source. It is shown that the discussion is only meaningful when ambiguities in the definitions of stress-energy tensor and energy density of a nonminimally coupled scalar are resolved. The three possible approaches are discussed with emphasis on the positivity of the respective energy densities and covariant conservation laws. The root of the ambiguities is traced to the energy localization problem for the gravitational field.

  1. Fluid/Gravity Correspondence with Scalar Field and Electromagnetic Field

    CERN Document Server

    Chou, Chia-Jui; Yang, Yi; Yuan, Pei-Hung

    2016-01-01

    We consider fluid/gravity correspondence in a general rotating black hole background with scalar and electromagnetic fields. Using the method of Petrov-like boundary condition, we show that the scalar and the electromagnetic fields contribute external forces to the dual Navier-Stokes equation and the rotation of black hole induces the Coriolis force.

  2. Generalized gravitational entropy of interacting scalar field and Maxwell field

    Directory of Open Access Journals (Sweden)

    Wung-Hong Huang

    2014-12-01

    Full Text Available The generalized gravitational entropy proposed recently by Lewkowycz and Maldacena is extended to the interacting real scalar field and Maxwell field system. Using the BTZ geometry we first investigate the case of free real scalar field and then show a possible way to calculate the entropy of the interacting scalar field. Next, we investigate the Maxwell field system. We exactly solve the wave equation and calculate the analytic value of the generalized gravitational entropy. We also use the Einstein equation to find the effect of backreaction of the Maxwell field on the area of horizon. The associated modified area law is consistent with the generalized gravitational entropy.

  3. Generalized gravitational entropy of interacting scalar field and Maxwell field

    Science.gov (United States)

    Huang, Wung-Hong

    2014-12-01

    The generalized gravitational entropy proposed recently by Lewkowycz and Maldacena is extended to the interacting real scalar field and Maxwell field system. Using the BTZ geometry we first investigate the case of free real scalar field and then show a possible way to calculate the entropy of the interacting scalar field. Next, we investigate the Maxwell field system. We exactly solve the wave equation and calculate the analytic value of the generalized gravitational entropy. We also use the Einstein equation to find the effect of backreaction of the Maxwell field on the area of horizon. The associated modified area law is consistent with the generalized gravitational entropy.

  4. Generalized gravitational entropy of interacting scalar field and Maxwell field

    Energy Technology Data Exchange (ETDEWEB)

    Huang, Wung-Hong, E-mail: whhwung@mail.ncku.edu.tw

    2014-12-12

    The generalized gravitational entropy proposed recently by Lewkowycz and Maldacena is extended to the interacting real scalar field and Maxwell field system. Using the BTZ geometry we first investigate the case of free real scalar field and then show a possible way to calculate the entropy of the interacting scalar field. Next, we investigate the Maxwell field system. We exactly solve the wave equation and calculate the analytic value of the generalized gravitational entropy. We also use the Einstein equation to find the effect of backreaction of the Maxwell field on the area of horizon. The associated modified area law is consistent with the generalized gravitational entropy.

  5. Age Crises, Scalar Fields, and the Apocalypse

    Science.gov (United States)

    Jackson, J. C.

    Recent observations suggest that Hubble's constant is large, to the extent that the oldest stars appear to have ages which are greater than the Hubble time, and that the Hubble expansion is slowing down, so that according to conventional cosmology the age of the Universe is less than the Hubble time. The concepts of weak and strong age crises (respectively t01/H0 and q0>0) are introduced. These observations are reconciled in models which are dynamically dominated by a homogeneous scalar field, corresponding to an ultra-light boson whose Compton wavelength is of the same order as the Hubble radius. Two such models are considered, an open one with vacuum energy comprising a conventional cosmological term and a scalar field component, and a flat one with a scalar component only, aimed respectively at weak and strong age crises. Both models suggest that anti-gravity plays a significant role in the evolution of the Universe.

  6. Gravitational waves from scalar field accretion

    CERN Document Server

    Núnez, Darío; Moreno, Claudia

    2011-01-01

    Our aim in this work is to outline some physical consequences of the interaction between black holes and scalar field halos in terms of gravitational waves. In doing so, the black hole is taken as a static and spherically symmetric gravitational source, {\\it i. e.} the Schwarzschild black hole, and we work within the test field approximation, considering that the scalar field lives in the curved space-time outside the black hole. We focused on the emission of gravitational waves when the black hole is perturbed by the surrounding scalar field matter. The symmetries of the spacetime and the simplicity of the matter source allow, by means of a spherical harmonic decomposition, to study the problem by means of a one dimensional description. Some properties of such gravitational waves are discussed as a function of the parameters of the infalling scalar field, and allow us to make the conjecture that the gravitational waves carry information on the type of matter that generated them.

  7. Scalar Field Theory on Fuzzy S^4

    CERN Document Server

    Medina, J; Medina, Julieta; Connor, Denjoe O'

    2003-01-01

    Scalar fields are studied on fuzzy $S^4$ and a solution is found for the elimination of the unwanted degrees of freedom that occur in the model. The resulting theory can be interpreted as a Kaluza-Klein reduction of CP^3 to S^4 in the fuzzy context.

  8. Cosmological evolution of a ghost scalar field

    OpenAIRE

    Sushkov, S. V.; Kim, S. -W

    2004-01-01

    We consider a scalar field with a negative kinetic term minimally coupled to gravity. We obtain an exact non-static spherically symmetric solution which describes a wormhole in cosmological setting. The wormhole is shown to connect two homogeneous spatially flat universes expanding with acceleration. Depending on the wormhole's mass parameter $m$ the acceleration can be constant (the de Sitter case) or infinitely growing.

  9. Black hole with a scalar field as a particle accelerator

    CERN Document Server

    Zaslavskii, O B

    2016-01-01

    We consider black holes with the background scalar field and test particles that can interact with this field directly. Then, particle collision near a black hole can lead to unbound energy $E_{c.m.}$ in the centre of mass frame (contrary to some recent claims in literature). This happens if one of particles is neutral whereas another one has nonzero scalar charge. Kinematically, two cases occur here. (i) A neutral particle approaches the horizon with the speed of light while the velocity of the charged one remains separated from it (this is direct analogue of the situation with collision of geodesic particles.). (ii) Both particles approach the horizon with the speed almost equal to that of light but with different rates. As a result, in both cases the relative velocity also approaches the speed of light, so that $E_{c.m.}$ $\\ $becomes unbound.

  10. Gravitational Gauge Interactions of Scalar Field

    Institute of Scientific and Technical Information of China (English)

    WU Ning

    2003-01-01

    Quantum gauge theory of gravity is formulated based on gauge principle. Because the Lagrangian hasstrict local gravitational gauge symmetry, gravitational gauge theory is a perturbatively renormalizable quantum theory.Gravitational gauge interactions of scalar field are studied in this paper. In quantum gauge theory of gravity, scalar fieldminimal couples to gravitational field through gravitational gauge covariant derivative. Comparing the Lagrangian forscalar field in quantum gauge theory of gravity with the corresponding Lagrangian in quantum fields in curved space-time, the definition for metric in curved space-time in geometry picture of gravity can be obtained, which is expressedby gravitational gauge field. In classical level, the Lagrangian and Hamiltonian approaches are also discussed.

  11. Challenging the Presence of Scalar Charge and Dipolar Radiation in Binary Pulsars

    CERN Document Server

    Yagi, Kent; Yunes, Nicolas

    2016-01-01

    Corrections to general relativity that introduce long-ranged scalar fields which are non-minimally coupled to curvature typically predict that neutron stars possess a non-trivial scalar field profile. An observer far from a star is most sensitive to the spherically-symmetric piece of this profile that decays linearly with the inverse of the distance, the so-called scalar charge, which is related to the emission of dipolar radiation from compact binaries. The presence of dipolar radiation has the potential to very strongly constrain extended theories of gravity. These facts may lead people to believe that gravitational theories with long-ranged scalar fields have already been constrained strongly from binary pulsar observations. Here we challenge this "lore" by investigating the decoupling limit of Gauss-Bonnet gravity as an example, in which the scalar field couples linearly to the Gauss-Bonnet density in the action. We prove a theorem that neutron stars in this theory cannot possess a scalar charge. Thus Gau...

  12. Two scalar field cosmology from coupled one-field models

    CERN Document Server

    Moraes, P H R S

    2014-01-01

    One possible description for the current accelerated expansion of the universe is quintessence dynamics. The basic idea of quintessence consists of analyzing cosmological scenarios driven by scalar fields. In this work we present some interesting features on the cosmological scenario obtained from the solutions of an effective two scalar field model in a flat space-time. This effective model was constructed by coupling two single scalar field systems in a nontrivial way via an extension method. The solutions related to the fields allowed us to compute analytical cosmological parameters. The behavior of these parameters are highlighted, as well as the different epochs obtained from them.

  13. Dynamical analysis in scalar field cosmology

    CERN Document Server

    Paliathanasis, Andronikos; Basilakos, Spyros; Barrow, John D

    2015-01-01

    A general method to extract exact cosmological solutions for scalar field dark energy in the presence of perfect fluids is presented. We use as a selection rule the existence of invariant transformations for the Wheeler De Witt (WdW) equation. We show that the existence of point transformation in which the WdW equation is invariant is equivalent to the existence of conservation laws for the field equations. Mathematically, the existence of extra integrals of motion indicates the existence of analytical solutions. We extend previous work by providing exact solutions for the Hubble parameter and the effective dark energy equation of state parameter for cosmologies containing a combination of perfect fluid and a scalar field whose self-interaction potential is a power of hyperbolic functions. Finally, we perform a dynamical analysis by studying the fixed points of the field equations using dimensionless variables. Amongst the variety of dynamical cases, we find that if the current cosmological model is Liouville...

  14. Interacting scalar fields in de Sitter space

    CERN Document Server

    Devaraj, G; Devaraj, Ganesh; Einhorn, Martin B

    1995-01-01

    We investigate the massless \\lambda \\phi^4 theory in de Sitter space. We argue that the infrared divergence associated with the free massless, minimally coupled scalar field in de Sitter space is not present when interactions are included because the field does not remain minimally coupled. This is essentially because \\xi=0 is not a fixed point of the renormalization group once interactions are included.

  15. The scalar field kernel in cosmological spaces

    Energy Technology Data Exchange (ETDEWEB)

    Koksma, Jurjen F; Prokopec, Tomislav [Institute for Theoretical Physics (ITP) and Spinoza Institute, Utrecht University, Postbus 80195, 3508 TD Utrecht (Netherlands); Rigopoulos, Gerasimos I [Helsinki Institute of Physics, University of Helsinki, PO Box 64, FIN-00014 (Finland)], E-mail: J.F.Koksma@phys.uu.nl, E-mail: T.Prokopec@phys.uu.nl, E-mail: gerasimos.rigopoulos@helsinki.fi

    2008-06-21

    We construct the quantum-mechanical evolution operator in the functional Schroedinger picture-the kernel-for a scalar field in spatially homogeneous FLRW spacetimes when the field is (a) free and (b) coupled to a spacetime-dependent source term. The essential element in the construction is the causal propagator, linked to the commutator of two Heisenberg picture scalar fields. We show that the kernels can be expressed solely in terms of the causal propagator and derivatives of the causal propagator. Furthermore, we show that our kernel reveals the standard light cone structure in FLRW spacetimes. We finally apply the result to Minkowski spacetime, to de Sitter spacetime and calculate the forward time evolution of the vacuum in a general FLRW spacetime.

  16. Charged scalar gravitational collapse in de Sitter spacetime

    CERN Document Server

    Zhang, Cheng-Yong; Zou, De-Cheng; Wang, Bin

    2015-01-01

    We study the charged scalar collapse in de Sitter spacetimes. With the electric charge, there is one more competitor to join the competition of dynamics in the gravitational collapse. We find that two factors can influence the electric charge. If we just adjust the charge-conjugation, the electric charge effect is always perturbative at the black hole threshold. The electric charge can also be influenced by the initial conditions of perturbations. These initial parameters can be tuned to control the competition in dynamics and present us new and rich physics in the process of gravitational collapse. We give physical explanations on these phenomena found in dynamics. Furthermore we show that the properties of the gravitational collapse are universal and do not depend on spacetime dimensions.

  17. Entanglement entropy for free scalar fields in AdS

    CERN Document Server

    Sugishita, Sotaro

    2016-01-01

    We compute entanglement entropy for free massive scalar fields in anti-de Sitter (AdS) space. The entangling surface is a minimal surface whose boundary is a sphere at the boundary of AdS. The entropy can be evaluated from the thermal free energy of the fields on a topological black hole by using the replica method. In odd-dimensional AdS, exact expressions of the Renyi entropy S_n are obtained for arbitrary n. We also evaluate 1-loop corrections coming from the scalar fields to holographic entanglement entropy. Applying the results, we compute the leading difference of entanglement entropy between two holographic CFTs related by a renormalization group flow triggered by a double trace deformation. The difference is proportional to the shift of a central charge under the flow.

  18. Extremal Kerr–Newman black holes with extremely short charged scalar hair

    Directory of Open Access Journals (Sweden)

    Shahar Hod

    2015-12-01

    Full Text Available The recently proved ‘no short hair’ theorem asserts that, if a spherically-symmetric static black hole has hair, then this hair (the external fields must extend beyond the null circular geodesic (the “photonsphere” of the corresponding black-hole spacetime: rfield>rnull. In this paper we provide compelling evidence that the bound can be violated by non-spherically symmetric hairy black-hole configurations. To that end, we analytically explore the physical properties of cloudy Kerr–Newman black-hole spacetimes – charged rotating black holes which support linearized stationary charged scalar configurations in their exterior regions. In particular, for given parameters {M,Q,J} of the central black hole, we find the dimensionless ratio q/μ of the field parameters which minimizes the effective lengths (radii of the exterior stationary charged scalar configurations (here {M,Q,J} are respectively the mass, charge, and angular momentum of the black hole, and {μ,q} are respectively the mass and charge coupling constant of the linearized scalar field. This allows us to prove explicitly that (non-spherically symmetric non-static composed Kerr–Newman-charged-scalar-field configurations can violate the no-short-hair lower bound. In particular, it is shown that extremely compact stationary charged scalar ‘clouds’, made of linearized charged massive scalar fields with the property rfield→rH, can be supported in the exterior spacetime regions of extremal Kerr–Newman black holes (here rfield is the peak location of the stationary scalar configuration and rH is the black-hole horizon radius. Furthermore, we prove that these remarkably compact stationary field configurations exist in the entire range s≡J/M2∈(0,1 of the dimensionless black-hole angular momentum. In particular, in the large-mass limit they are characterized by the simple dimensionless ratio q/μ=(1−2s2/(1−s2.

  19. Stability of the extremal Reissner-Nordström black hole to charged scalar perturbations

    International Nuclear Information System (INIS)

    The stability of Reissner-Nordström black holes to neutral (gravitational and electromagnetic) perturbations was established almost four decades ago. However, the stability of these charged black holes under charged perturbations has remained an open question due to the well-known phenomena of superradiant scattering: A charged scalar field impinging on a charged Reissner-Nordström black hole can be amplified as it scatters off the hole. If the incident field has a non-zero rest mass, then the mass term effectively works as a mirror, preventing the energy extracted from the hole from escaping to infinity. One may suspect that such superradiant amplification of charged fields in Reissner-Nordström spacetimes may lead to an instability of these charged black holes (in as much the same way that rotating Kerr black holes are unstable under rotating scalar perturbations). However, we show here that, for extremal Reissner-Nordström black holes, the two conditions which are required in order to trigger a possible superradiant instability [namely: (1) the existence of a trapping potential well outside the black hole, and (2) superradiant amplification of the trapped modes] cannot be satisfied simultaneously. Our results thus support the stability of extremal Reissner-Nordström black holes to charged scalar perturbations.

  20. Euclidean wormholes with minimally coupled scalar fields

    International Nuclear Information System (INIS)

    A detailed study of quantum and semiclassical Euclidean wormholes for Einstein's theory with a minimally coupled scalar field has been performed for a class of potentials. Massless, constant, massive (quadratic in the scalar field) and inverse (linear) potentials admit the Hawking and Page wormhole boundary condition both in the classically forbidden and allowed regions. An inverse quartic potential has been found to exhibit a semiclassical wormhole configuration. Classical wormholes under a suitable back-reaction leading to a finite radius of the throat, where the strong energy condition is satisfied, have been found for the zero, constant, quadratic and exponential potentials. Treating such classical Euclidean wormholes as an initial condition, a late stage of cosmological evolution has been found to remain unaltered from standard Friedmann cosmology, except for the constant potential which under the back-reaction produces a term like a negative cosmological constant. (paper)

  1. Reconstructing bidimensional scalar field theory models

    Energy Technology Data Exchange (ETDEWEB)

    Flores, Gabriel H.; Svaiter, N.F. [Centro Brasileiro de Pesquisas Fisicas (CBPF), Rio de Janeiro, RJ (Brazil)]. E-mail: gflores@cbpf.br; nfuxsvai@cbpf.br

    2001-07-01

    In this paper we review how to reconstruct scalar field theories in two dimensional spacetime starting from solvable Scrodinger equations. Theree different Schrodinger potentials are analyzed. We obtained two new models starting from the Morse and Scarf II hyperbolic potencials, the U ({theta}) {theta}{sup 2} In{sup 2} ({theta}{sup 2}) model and U ({theta}) = {theta}{sup 2} cos{sup 2} (In({theta}{sup 2})) model respectively. (author)

  2. Cosmological scalar field perturbations can grow

    Science.gov (United States)

    Alcubierre, Miguel; de la Macorra, Axel; Diez-Tejedor, Alberto; Torres, José M.

    2015-09-01

    It has been argued that the small perturbations to the homogeneous and isotropic configurations of a canonical scalar field in an expanding universe do not grow. We show that this is not true in general, and clarify the root of the misunderstanding. We revisit a simple model in which the zero mode of a free scalar field oscillates with high frequency around the minimum of the potential. Under this assumption the linear perturbations grow like those in the standard cold dark matter scenario, but with a Jeans length at the scale of the Compton wavelength of the scalar particle. Contrary to previous analyses in the literature our results do not rely on time averages and/or fluid identifications, and instead we solve both analytically (in terms of a well-defined series expansion) and numerically the linearized Einstein-Klein-Gordon system. Also, we use gauge-invariant fields, which makes the physical analysis more transparent and simplifies the comparison with previous works carried out in different gauges. As a byproduct of this study we identify a time-dependent modulation of the different physical quantities associated to the background as well as the perturbations with potential observational consequences in dark matter models.

  3. Reconciling $(g-2)_\\mu$ and charged lepton flavour violating processes through a doubly charged scalar

    CERN Document Server

    Chakrabortty, Joydeep; Mondal, Subhadeep; Srivastava, Tripurari

    2015-01-01

    In this work, we investigate the phenomenological consequences of a doubly charged scalar which may belong to different uncoloured scalar multiplets. This doubly charged scalar couples to the charged leptons as well as gauge bosons, which we parametrize in a model independent way. Restricting ourselves in the regime of conserved charged-parity (CP), we assume only a few non-zero Yukawa couplings ($y_{\\mu \\ell}$, where $\\ell=e,\\mu,\\tau$) between the doubly charged scalar and the charged leptons. Our choices allow the doubly charged scalar to impinge low-energy processes like anomalous magnetic moment of muon and a few possible charged lepton flavour violating (CLFV) processes. These same Yukawa couplings are also instrumental in producing same-sign di-lepton signatures at the LHC. In this article we examine the impact of individual contributions from the diagonal and off-diagonal Yukawa couplings in the light of muon $(g-2)$ excess. Subsequently, we use the derived information to inquire the possible CLFV proc...

  4. Casimir Effect of Scalar Massive Field

    CERN Document Server

    Mobassem, Sonia

    2014-01-01

    The energy momentum tensor is used to introduce the Casimir force of the massive scalar field acting on a nonpenetrating surface. This expression can be used to evaluate the vacuum force by employing the appropriate field operators. To simplify our formalism we also relates the vacuum force expression to the imaginary part of the Green function via the fluctuation dissipation theorem and Kubo formula. This allows one to evaluate the vacuum force without resorting to the process of field quantization. These two approaches are used to calculate the attractive force between two nonpenetrating plates. Special attention is paid to the generalization of the formalism to D + 1 space-time dimensions.

  5. Finite temperature Casimir effect for massive scalars in a magnetic field

    CERN Document Server

    Erdas, Andrea

    2013-01-01

    The finite temperature Casimir effect for a charged, massive scalar field confined between very large, perfectly conducting parallel plates is studied using the zeta function regularization technique. The scalar field satisfies Dirichlet boundary conditions at the plates and a magnetic field perpendicular to the plates is present. Four equivalent expressions for the zeta function are obtained, which are exact to all orders in the magnetic field strength, temperature, scalar field mass, and plate distance. The zeta function is used to calculate the Helmholtz free energy of the scalar field and the Casimir pressure on the plates, in the case of high temperature, small plate distance, strong magnetic field and large scalar mass. In all cases, simple analytic expressions of the zeta function, free energy and pressure are obtained, which are very accurate and valid for practically all values of temperature, plate distance, magnetic field and mass.

  6. Quantum tunneling from scalar fields in rotating black strings

    CERN Document Server

    Gohar, H

    2011-01-01

    Using the Hamilton-Jacobi method of quantum tunneling and complex path integration, we study Hawking radiation of scalar particles from rotating black strings. We discuss tunneling of both charged and uncharged scalar particles from the event horizons. For this purpose, we use the Klein-Gordon equation and find the tunneling probability of outging scalar particles. The procedure gives Hawking temperature for rotating charged black strings as well.

  7. Quantum tunneling from scalar fields in rotating black strings

    Science.gov (United States)

    Gohar, H.; Saifullah, K.

    2013-08-01

    Using the Hamilton-Jacobi method of quantum tunneling and complex path integration, we study Hawking radiation of scalar particles from rotating black strings. We discuss tunneling of both charged and uncharged scalar particles from the event horizons. For this purpose, we use the Klein-Gordon equation and find the tunneling probability of outgoing scalar particles. The procedure gives Hawking temperature for rotating charged black strings as well.

  8. Scalar fields properties for flat galactic rotation curves

    CERN Document Server

    Fay, S

    2004-01-01

    The whole class of minimally coupled and massive scalar fields which may be responsible for flattening of galactic rotation curves is found. An interesting relation with a class of scalar-tensor theories able to isotropise anisotropic models of Universe is shown. The resulting metric is found and its stability and scalar field properties are tested with respect to the presence of a second scalar field or a small perturbation of the rotation velocity at galactic outer radii.

  9. Twinlike models in scalar field theories

    International Nuclear Information System (INIS)

    This work deals with the presence of defect structures in models described by a real scalar field in a diversity of scenarios. The defect structures that we consider are static solutions of the equations of motion that depend on a single spatial dimension. We search for different models, which support the same defect solution, with the very same energy density. We work in flat spacetime, where we introduce and investigate a new class of models. We also work in curved spacetime, within the braneworld context, with a single extra dimension of infinite extent, and there we show how the brane is formed from the static field configuration.

  10. Thermodynamic phase structure of charged anti-de Sitter scalar-tensor black holes

    International Nuclear Information System (INIS)

    When electromagnetic field with nonlinear lagrangian acts as a source of gravity the no-scalar-hair theorems can be eluded and black holes with non-trivial scalar field can be found in scalar tensor theories. Black holes with secondary scalar hair exist also when a cosmological constant is added in the theory. The thermodynamics of black holes in anti-de Sitter (AdS) space-time has attracted considerable interest due to the AdS/CFT conjecture. A natural question that arises is whether the non-trivial scalar field would alter the black-hole thermodynamical phase structure. In the current work we present the phase structure of charged hairy black holes coupled to nonlinear Born-Infeld electrodynamics in canonical ensemble which is naturally related to AdS space-time. In certain regions of the parameter space we find the existence of a first-order phase transition between small and very large black holes. An unexpected result is that for a small subinterval of charge values two phase transitions are observed – one of zeroth and one of first order

  11. Generalized Gravitational Entropy of Interacting Scalar Field and Maxwell Field

    CERN Document Server

    Huang, Wung-Hong

    2014-01-01

    The generalized gravitational entropy proposed by Lewkowycz and Maldacena in recent is extended to the interacting real scalar field and Maxwell field system. Using the BTZ geometry we first investigate the case of free real scalar field and then show a possible way to calculate the entropy of the interacting scalar field. Next, we investigate the Maxwell field system. We exactly solve the wave equation and calculate the analytic value of the generalized gravitational entropy. We also use the Einstein equation to find the effect of backreaction of the Maxwell field on the spacetime. The associated modified area law is consistent with the generalized gravitational entropy. Our investigations have not found the unexpected anomalous surface term.

  12. Vacuum polarization of a scalar field in wormhole spacetimes

    CERN Document Server

    Popov, A A; Popov, Arkadii A.; Sushkov, Sergey V.

    2001-01-01

    An analitical approximation of $$ for a scalar field in a static spherically symmetric wormhole spacetime is obtained. The scalar field is assumed to be both massive and massless, with an arbitrary coupling $\\xi$ to the scalar curvature, and in a zero temperature vacuum state.

  13. The Einstein-scalar field constraints on asymptotically Euclidean manifolds

    CERN Document Server

    Choquet-Bruhat, Y; Pollack, D; Choquet-Bruhat, Yvonne; Isenberg, James; Pollack, Daniel

    2005-01-01

    We use the conformal method to obtain solutions of the Einstein-scalar field gravitational constraint equations. Handling scalar fields is a bit more challenging than handling matter fields such as fluids, Maxwell fields or Yang-Mills fields, because the scalar field introduces three extra terms into the Lichnerowicz equation, rather than just one. Our proofs are constructive and allow for arbitrary dimension (>2) as well as low regularity initial data.

  14. Scalar and electromagnetic fields of static sources in higher dimensional Majumdar-Papapetrou spacetimes

    Science.gov (United States)

    Frolov, Valeri P.; Zelnikov, Andrei

    2012-03-01

    We study massless scalar and electromagnetic fields from static sources in a static higher-dimensional spacetime. Exact expressions for static Green’s functions for such problems are obtained in the background of the Majumdar-Papapetrou solutions of the Einstein-Maxwell equations. Using this result, we calculate the force between two scalar or electric charges in the presence of one or several extremally charged black holes in equilibrium in the higher-dimensional spacetime.

  15. Scalar Quantum Field Theory on Fractals

    CERN Document Server

    Kar, Arnab

    2011-01-01

    We construct a family of measures for random fields based on the iterated subdivision of simple geometric shapes (triangles, squares, tetrahedrons) into a finite number of similar shapes. The intent is to construct continuum limits of scale invariant scalar field theories, by imitating Wiener's construction of the measure on the space of functions of one variable. These are Gaussian measures, except for one example of a non-Gaussian fixed point for the Ising model on a fractal. In the continuum limits what we construct have correlation functions that vary as a power of distance. In most cases this is a positive power (as for the Wiener measure) but we also find a few examples with negative exponent. In all cases the exponent is an irrational number, which depends on the particular subdivision scheme used. This suggests that the continuum limits corresponds to quantum field theories (random fields) on spaces of fractional dimension.

  16. Induced Gravity I: Real Scalar Field

    CERN Document Server

    Einhorn, Martin B

    2016-01-01

    We show that classically scale invariant gravity coupled to a single scalar field can undergo dimensional transmutation and generate an effective Einstein-Hilbert action for gravity, coupled to a massive dilaton. The same theory has an ultraviolet fixed point for coupling constant ratios such that all couplings are asymptotically free. However the catchment basin of this fixed point does not include regions of coupling constant parameter space compatible with locally stable dimensional transmutation. We believe that the desirable outcome may obtain in more complicated theories with non-Abelian gauge interactions.

  17. Scalar field collapse with negative cosmological constant

    CERN Document Server

    Baier, R; Stricker, S A

    2014-01-01

    The formation of black holes or naked singularities is studied in a model in which a homogeneous time-dependent scalar field with an exponential potential couples to four dimensional gravity with negative cosmological constant. An analytic solution is derived and its consequences are discussed. The model depends only on one free parameter which determines the equation of state and decides the fate of the spacetime. Depending on the value of this parameter the collapse ends in a black hole or a naked singularity. The latter case violates the cosmic censorship conjecture.

  18. Global integrability of cosmological scalar fields

    CERN Document Server

    Maciejewski, Andrzej J; Stachowiak, Tomasz; Szydlowski, Marek

    2008-01-01

    We investigate the Liouvillian integrability of Hamiltonian systems describing a universe filled with a scalar field (possibly complex). The tool used is the differential Galois group approach, as introduced by Morales-Ruiz and Ramis. The main result is that the generic systems with minimal coupling are non-integrable, although there still exist some values of parameters for which integrability remains undecided; the conformally coupled systems are only integrable in four known cases. We also draw a connection with chaos present in such cosmological models, and the issues of integrability restricted to the real domain.

  19. Scalar field dark matter and the Higgs field

    OpenAIRE

    Bertolami, O.; Catarina Cosme; Rosa, João G.

    2016-01-01

    We discuss the possibility that dark matter corresponds to an oscillating scalar field coupled to the Higgs boson. We argue that the initial field amplitude should generically be of the order of the Hubble parameter during inflation, as a result of its quasi-de Sitter fluctuations. This implies that such a field may account for the present dark matter abundance for masses in the range 10−6–10−4eV, if the tensor-to-scalar ratio is within the range of planned CMB experiments. We show that such ...

  20. Dynamical analysis in scalar field cosmology

    Science.gov (United States)

    Paliathanasis, Andronikos; Tsamparlis, Michael; Basilakos, Spyros; Barrow, John D.

    2015-06-01

    We give a general method to find exact cosmological solutions for scalar-field dark energy in the presence of perfect fluids. We use the existence of invariant transformations for the Wheeler De Witt (WdW) equation. We show that the existence of a point transformation under which the WdW equation is invariant is equivalent to the existence of conservation laws for the field equations, which indicates the existence of analytical solutions. We extend previous work by providing exact solutions for the Hubble parameter and the effective dark-energy equation of state parameter for cosmologies containing a combination of perfect fluid and a scalar field whose self-interaction potential is a power of hyperbolic functions. We find solutions explicitly when the perfect fluid is radiation or cold dark matter and determine the effects of nonzero spatial curvature. Using the Planck 2015 data, we determine the evolution of the effective equation of state of the dark energy. Finally, we study the global dynamics using dimensionless variables. We find that if the current cosmological model is Liouville integrable (admits conservation laws) then there is a unique stable point which describes the de-Sitter phase of the universe.

  1. Higgs and gravitational scalar fields together induce Weyl gauge

    OpenAIRE

    Scholz, Erhard

    2014-01-01

    A common biquadratic potential for the Higgs field $h$ and an additional scalar field $\\phi$, non minimally coupled to gravity, is considered in locally scale symmetric approaches to standard model fields in curved spacetime. A common ground state of the two scalar fields exists and couples both fields to gravity, more precisely to scalar curvature $R$. In Einstein gauge ($\\phi = const$, often called "Einstein frame"), also $R$ is scaled to a constant. This condition makes perfect sense, even...

  2. Scalar field self-force effects on a particle orbiting a Reissner-Nordstrom black hole

    CERN Document Server

    Bini, Donato; Geralico, Andrea

    2016-01-01

    Scalar field self-force effects on a scalar charge orbiting a Reissner-Nordstr\\"om black hole are investigated. The scalar wave equation is solved analytically in a post-Newtonian framework, and the solution is used to compute the self-field as well as the components of the self-force at the particle's location up to 7.5 post-Newtonian order. The energy fluxes radiated to infinity and down the hole are also evaluated. Comparison with previous numerical results in the Schwarzschild case shows a good agreement in both strong-field and weak-field regimes.

  3. Scalar field dark matter and the Higgs field

    Directory of Open Access Journals (Sweden)

    O. Bertolami

    2016-08-01

    Full Text Available We discuss the possibility that dark matter corresponds to an oscillating scalar field coupled to the Higgs boson. We argue that the initial field amplitude should generically be of the order of the Hubble parameter during inflation, as a result of its quasi-de Sitter fluctuations. This implies that such a field may account for the present dark matter abundance for masses in the range 10−6–10−4eV, if the tensor-to-scalar ratio is within the range of planned CMB experiments. We show that such mass values can naturally be obtained through either Planck-suppressed non-renormalizable interactions with the Higgs boson or, alternatively, through renormalizable interactions within the Randall–Sundrum scenario, where the dark matter scalar resides in the bulk of the warped extra-dimension and the Higgs is confined to the infrared brane.

  4. Scalar field dark matter and the Higgs field

    Science.gov (United States)

    Bertolami, O.; Cosme, Catarina; Rosa, João G.

    2016-08-01

    We discuss the possibility that dark matter corresponds to an oscillating scalar field coupled to the Higgs boson. We argue that the initial field amplitude should generically be of the order of the Hubble parameter during inflation, as a result of its quasi-de Sitter fluctuations. This implies that such a field may account for the present dark matter abundance for masses in the range 10-6-10-4eV, if the tensor-to-scalar ratio is within the range of planned CMB experiments. We show that such mass values can naturally be obtained through either Planck-suppressed non-renormalizable interactions with the Higgs boson or, alternatively, through renormalizable interactions within the Randall-Sundrum scenario, where the dark matter scalar resides in the bulk of the warped extra-dimension and the Higgs is confined to the infrared brane.

  5. Scalar Field Theories with Polynomial Shift Symmetries

    CERN Document Server

    Griffin, Tom; Horava, Petr; Yan, Ziqi

    2014-01-01

    We continue our study of naturalness in nonrelativistic QFTs of the Lifshitz type, focusing on scalar fields that can play the role of Nambu-Goldstone (NG) modes associated with spontaneous symmetry breaking. Such systems allow for an extension of the constant shift symmetry to a shift by a polynomial of degree $P$ in spatial coordinates. These "polynomial shift symmetries" in turn protect the technical naturalness of modes with a higher-order dispersion relation, and lead to a refinement of the proposed classification of infrared Gaussian fixed points available to describe NG modes in nonrelativistic theories. Generic interactions in such theories break the polynomial shift symmetry explicitly to the constant shift. It is thus natural to ask: Given a Gaussian fixed point with polynomial shift symmetry of degree $P$, what are the lowest-dimension operators that preserve this symmetry, and deform the theory into a self-interacting scalar field theory with the shift symmetry of degree $P$? To answer this (essen...

  6. Massive scalar field evolution in de Sitter

    CERN Document Server

    Markkanen, Tommi

    2016-01-01

    The behaviour of a massive, non-interacting and non-minimally coupled quantised scalar field in an expanding de Sitter background is investigated by solving the field evolution for an arbitrary initial state. In this approach there is no need to choose a vacuum in order to provide a definition for particle states. We conclude that the expanding de Sitter space is a stable equilibrium configuration under small perturbations of the initial conditions. Depending on the initial state, the energy density can approach its asymptotic value from above or below, the latter of which implies a violation of the weak energy condition. The backreaction of the quantum corrections can therefore lead to a phase of super-acceleration also in the non-interacting massive case.

  7. Imprint of thawing scalar fields on large scale galaxy overdensity

    CERN Document Server

    Dinda, Bikash R

    2016-01-01

    We calculate the observed galaxy power spectrum for the thawing class of scalar field models taking into account various general relativistic corrections that occur on very large scales. As we need to consider the fluctuations in scalar field on these large scales, the general relativistic corrections in thawing scalar field models are distinctly different from $\\Lambda$CDM and the difference can be upto $15-20\\%$ at some scales. Also there is an interpolation between suppression and enhancement of power in scalar field models compared to the $\\Lambda$CDM model on smaller scales and this happens in a specific redshift range that is quite robust to the form of the scalar field potentials or the choice of different cosmological parameters. This can be useful to distinguish scalar field models from $\\Lambda$CDM with future optical/radio surveys.

  8. Massive basketball diagram for a thermal scalar field theory

    Science.gov (United States)

    Andersen, Jens O.; Braaten, Eric; Strickland, Michael

    2000-08-01

    The ``basketball diagram'' is a three-loop vacuum diagram for a scalar field theory that cannot be expressed in terms of one-loop diagrams. We calculate this diagram for a massive scalar field at nonzero temperature, reducing it to expressions involving three-dimensional integrals that can be easily evaluated numerically. We use this result to calculate the free energy for a massive scalar field with a φ4 interaction to three-loop order.

  9. Lagrange Multipliers and Third Order Scalar-Tensor Field Theories

    CERN Document Server

    Horndeski, Gregory W

    2016-01-01

    In a space of 4-dimensions, I will examine constrained variational problems in which the Lagrangian, and constraint scalar density, are concomitants of a (pseudo-Riemannian) metric tensor and its first two derivatives. The Lagrange multiplier for these constrained extremal problems will be a scalar field. For suitable choices of the Lagrangian, and constraint, we can obtain Euler-Lagrange equations which are second order in the scalar field and third order in the metric tensor. The effect of disformal transformations on the constraint Lagrangians, and their generalizations, is examined. This will yield other second order scalar-tensor Lagrangians which yield field equations which are at most of third order. No attempt is made to construct all possible third order scalar-tensor Euler-Lagrange equations in a 4-space, although nine classes of such field equations are presented. Two of these classes admit subclasses which yield conformally invariant field equations. A few remarks on scalar-tensor-connection theor...

  10. Self-interacting complex scalar field as dark matter

    International Nuclear Information System (INIS)

    We study the viability of a a complex scalar field χ with self-interacting potential V = m0χ/2|χ|2+h|χ|4 as dark matter. Due to the self interaction, the scalar field forms a Bose-Einstein condensate at early times that represents dark matter. The self interaction is also responsible of quantum corrections to the scalar field mass that naturally give the dark matter domination at late times without any fine tuning on the energy density of the scalar field at early times. Finally the properties of the spherically symmetric dark matter halos are also discussed.

  11. One-loop quantum corrections to cosmological scalar field potentials

    CERN Document Server

    Arbey, A; Arbey, Alexandre; Mahmoudi, Farvah

    2007-01-01

    We study the loop corrections to potentials of complex or coupled real scalar fields used in cosmology to account for dark energy, dark matter or dark fluid. We show that the SUGRA quintessence and dark matter scalar field potentials are stable against the quantum fluctuations, and we propose solutions to the instability of the potentials of coupled quintessence and dark fluid scalar fields. We also find that a coupling to fermions is very restricted, unless this coupling has a structure which already exists in the scalar field potential or which can be compensated by higher order corrections. Finally, we study the influence of the curvature and kinetic term corrections.

  12. Inflationary solutions in the nonminimally coupled scalar field theory

    Science.gov (United States)

    Koh, Seoktae; Kim, Sang Pyo; Song, Doo Jong

    2005-08-01

    We study analytically and numerically the inflationary solutions for various type scalar potentials in the nonminimally coupled scalar field theory. The Hamilton-Jacobi equation is used to deal with nonlinear evolutions of inhomogeneous spacetimes and the long-wavelength approximation is employed to find the homogeneous solutions during an inflation period. The constraints that lead to a sufficient number of e-folds, a necessary condition for inflation, are found for the nonminimal coupling constant and initial conditions of the scalar field for inflation potentials. In particular, we numerically find an inflationary solution in the new inflation model of a nonminimal scalar field.

  13. Thermal Inflation with a Thermal Waterfall Scalar Field Coupled to a Light Spectator Scalar Field

    CERN Document Server

    Rumsey, Arron

    2016-01-01

    This thesis begins with an introduction to the state of the art of modern Cosmology. The field of Particle Cosmology is then introduced and explored, in particular with regard to the study of cosmological inflation. We then introduce a new model of Thermal Inflation, in which the mass of the thermal waterfall field responsible for the inflation is dependent on a light spectator scalar field. The model contains a variety of free parameters, two of which control the power of the coupling term and the non-renormalizable term. We use the $\\delta N$ formalism to investigate the "end of inflation" and modulated decay scenarios in turn to see whether they are able to produce the dominant contribution to the primordial curvature perturbation $\\zeta$. We constrain the model and then explore the parameter space. We explore key observational signatures, such as non-Gaussianity, the scalar spectral index and the running of the scalar spectral index. We find that for some regions of the parameter space, the ability of the...

  14. Scalar field dark matter: behavior around black holes

    International Nuclear Information System (INIS)

    We present the numerical evolution of a massive test scalar fields around a Schwarzschild space-time. We proceed by using hyperboloidal slices that approach future null infinity, which is the boundary of scalar fields, and also demand the slices to penetrate the event horizon of the black hole. This approach allows the scalar field to be accreted by the black hole and to escape toward future null infinity. We track the evolution of the energy density of the scalar field, which determines the rate at which the scalar field is being diluted. We find polynomial decay of the energy density of the scalar field, and use it to estimate the rate of dilution of the field in time. Our findings imply that the energy density of the scalar field decreases even five orders of magnitude in time scales smaller than a year. This implies that if a supermassive black hole is the Schwarzschild solution, then scalar field dark matter would be diluted extremely fast

  15. Novel Localized Excitations of Nonlinear Coupled Scalar Fields

    Institute of Scientific and Technical Information of China (English)

    ZHU Ren-Gui; LI Jin-Hua; WANG An-Min; WU Huang-Jiao

    2008-01-01

    Some extended solution mapping relations of the nonlinear coupled scalar field and the well-known φ4 model are presented. Simultaneously, inspired by the new solutions of the famous φ4 model recently proposed by Jia, Huang and Lou, five kinds of new localized excitations of the nonlinear coupled scalar field (NCSF) system are obtained.

  16. Effective Hamiltonian for non-minimally coupled scalar fields

    OpenAIRE

    Mese, Emine; Pirinccioglu, Nurettin; Acikgoz, Irfan; Binbay, Figen

    2006-01-01

    Performing a relativistic approximation as the generalization to a curved spacetime of the flat space Klein-Gordon equation, an effective Hamiltonian which includes non-minimial coupling between gravity and scalar field and also quartic self-interaction of scalar field term is obtained.

  17. Decoding the hologram: Scalar fields interacting with gravity

    CERN Document Server

    Kabat, Daniel

    2013-01-01

    We construct smeared CFT operators which represent a scalar field in AdS interacting with gravity. The guiding principle is micro-causality: scalar fields should commute with themselves at spacelike separation. To O(1/N) we show that a correct and convenient criterion for constructing the appropriate CFT operators is to demand micro-causality in a three-point function with a boundary Weyl tensor and another boundary scalar. The resulting bulk observables transform in the correct way under AdS isometries and commute with boundary scalar operators at spacelike separation, even in the presence of metric perturbations.

  18. Effective field theory of quantum gravity coupled to scalar electrodynamics

    Science.gov (United States)

    Ibiapina Bevilaqua, L.; Lehum, A. C.; da Silva, A. J.

    2016-05-01

    In this work, we use the framework of effective field theory to couple Einstein’s gravity to scalar electrodynamics and determine the renormalization of the model through the study of physical processes below Planck scale, a realm where quantum mechanics and general relativity are perfectly compatible. We consider the effective field theory up to dimension six operators, corresponding to processes involving one-graviton exchange. Studying the renormalization group functions, we see that the beta function of the electric charge is positive and possesses no contribution coming from gravitational interaction. Our result indicates that gravitational corrections do not alter the running behavior of the gauge coupling constants, even if massive particles are present.

  19. Born-Infeld Black Holes Coupled to a Massive Scalar Field

    Science.gov (United States)

    Georgieva, Daniela A.; Stefanov, Ivan Zh.; Yazadjiev, Stoytcho S.; Todorov, Michail D.

    Born-Infeld black holes in the scalar-tensor theories of gravity with massless scalar field have been recently obtained [I. Stefanov, S. Yazadjiev and M. Todorov, Phys. Rev. D 75 (2007) 084036; Mod. Phys. Lett. A. 23(34) (2008) 2915; Class. Quantum Gravity 26 (2009) 015006]. The aim of the current paper is to study the effect of the inclusion of a potential for the scalar field in the theory, through a combination of analytical techniques and numerical methods. The black holes coupled to a massive scalar field have richer causal structure in comparison to the massless scalar field case. In the former case, the black holes may have a second, inner horizon. The presence of potential for the scalar field allows the existence of extremal black holes for certain values of the mass of the scalar field and the magnetic (electric) charge of the black hole. The solutions are stable against spherically symmetric perturbations. Arguments in favor of the general stability of the solutions coming from the application of the "turning point" method are also presented.

  20. Covariant and gauge-invariant linear scalar perturbations in multiple scalar field cosmologies

    CERN Document Server

    Alho, Artur

    2013-01-01

    We derive a set of equations monitoring the evolution of covariant and gauge-invariant linear scalar perturbations of Friedman-Lema\\^itre-Robertson-Walker models with multiple interacting non-linear scalar fields. We use a dynamical systems' approach in order to perform a stability analysis for some classes of scalar field potentials. In particular, using a recent approximation for the inflationary dynamics of the background solution, we derive conditions under which homogenization occurs for chaotic (quadratic and quartic potentials) and new inflation. We also prove a cosmic no-hair result for power-law inflation and its generalisation for two scalar fields with independent exponential potentials (assisted power-law inflation).

  1. Fundamental scalar fields and the dark side of the universe

    CERN Document Server

    Mychelkin, Eduard G

    2015-01-01

    Starting with geometrical premises, we infer the existence of fundamental cosmological scalar fields. We then consider physically relevant situations in which spacetime metric is induced by one or, in general, by two scalar fields, in accord with the Papapetrou algorithm. The first of these fields, identified with dark energy, has exceedingly small but finite (subquantum) Hubble mass scale (~ 10^-33 eV), and might be represented as a neutral superposition of quasi-static electric fields. The second field is identified with dark matter as an effectively scalar conglomerate composed of primordial neutrinos and antineutrinos in a special tachyonic state.

  2. Searching for Chameleon-like Scalar Fields

    CERN Document Server

    Levshakov, S A; Kozlov, M G; Lapinov, A V; Henkel, C; Reimers, D; Sakai, T; Agafonova, I I

    2010-01-01

    Using the 32-m Medicina, 45-m Nobeyama, and 100-m Effelsberg telescopes we found a statistically significant velocity offset Delta V = 27 +/- 3 m/s (1sigma) between the inversion transition in NH3(1,1) and low-J rotational transitions in N2H+(1-0) and HC3N(2-1) arising in cold and dense molecular cores in the Milky Way. Systematic shifts of the line centers caused by turbulent motions and velocity gradients, possible non-thermal hyperfine structure populations, pressure and optical depth effects are shown to be lower than or about 1 m/s and thus can be neglected in the total error budget. The reproducibility of Delta V at the same facility (Effelsberg telescope) on a year-to-year basis is found to be very good. Since the frequencies of the inversion and rotational transitions have different sensitivities to variations in mu = m_e/m_p, the revealed non-zero Delta V may imply that mu changes when measured at high (terrestrial) and low (interstellar) matter densities as predicted by chameleon-like scalar field m...

  3. Scalarization

    OpenAIRE

    Korf, Lisa A.; Wets, Roger J.-B.

    2000-01-01

    Random lsc (lower semicontinuous) functions can be indentified with a vector-valued random variable by means of an appropriate scalarization. It is shown that stationarity, ergodicity and independence properties are preserved by this scalarization. The scalarization is exploited to obtain an lsc version of the conditional expectation of a random lsc function.

  4. Hawking radiation of scalars from charged accelerating and rotating black holes with NUT parameter

    CERN Document Server

    Jan, Khush

    2013-01-01

    We study the quantum tunneling of scalars from charged accelerating and rotating black hole with NUT parameter. For this purpose we use the charged Klein-Gordon equation. We apply WKB approximation and the Hamilton-Jacobi method to solve charged the Klein-Gordon equation. We find the tunneling probability of outgoing charged scalars from the event horizon of this black hole, and hence the Hawking temperature for this black hole.

  5. Charged Scalar Phenomenology in the Bilinear R-Parity Breaking Model

    CERN Document Server

    Ferrandis, J

    1998-01-01

    We consider the charged scalar boson phenomenology in the bilinear R-parity breaking model which induces a mixing between staus and the charged Higgs boson. The charged Higgs boson mass can be lower than expected in the MSSM, even before including radiative corrections. The R-parity violating decay rates can be comparable or even bigger than the R-parity conserving ones. These features could have implications for charged supersymmetric scalar boson searches at future accelerators.

  6. Fundamental scalar fields and the dark side of the universe

    OpenAIRE

    Mychelkin, Eduard G.; Makukov, Maxim A.

    2015-01-01

    Starting with geometrical premises, we infer the existence of fundamental cosmological scalar fields. We then consider physically relevant situations in which spacetime metric is induced by one or, in general, by two scalar fields, in accord with the Papapetrou algorithm. The first of these fields, identified with dark energy, has exceedingly small but finite (subquantum) Hubble mass scale (~ 10^-33 eV), and might be represented as a neutral superposition of quasi-static electric fields. The ...

  7. GFFD: Generalized free-form deformation with scalar fields

    Institute of Scientific and Technical Information of China (English)

    秦绪佳; 华炜; 方向; 鲍虎军; 彭群生

    2003-01-01

    The novel free-form deformation(FFD) technique presented in the paper uses scalar fields defined by skeletons with arbitrary topology. The technique embeds objects into the scalar field by assigning a field value to each point of the objects. When the space of the skeleton is changed, the distribution of the scalar field changes accordingly, which implicitly defines a deformation of the space. The generality of skeletons assures that the technique can freely define deformable regions to produce a broader range of shape deformations.

  8. GFFD: Generalized free-form deformation with scalar fields

    Institute of Scientific and Technical Information of China (English)

    秦绪佳; 华炜; 方向; 鲍虎军; 彭群生

    2003-01-01

    The novel free-form deformation (FFD) technique presented in the paper uses scalar fields definedby skeletons with arbitrary topology. The technique embeds objects into the scalar field by assigning a field value to each point of the objects. When the space of the skeleton is changed, the distribution of the scalar field changes accordingly, which implicitly defines a deformation of the space. The generality of skeletons assures that the technique can freely define deformable regions to produce a broader range of shape deformations.

  9. Fast-roll solutions from two scalar field inflation

    CERN Document Server

    Santos, J R L

    2015-01-01

    The cosmological equations of motion of scalar fields are commonly not easy to be analytically solved, which makes necessary to use approximation methods, as the {\\it slow-roll} regime. In such an approximation one considers the scalar field potentials to be nearly flat. On the other hand, the so called {\\it fast-roll} regime considers exactly flat potentials. Our purpose in this work is to obtain solutions for a two scalar field quintessence model in the fast-roll regime. Cosmological interpretations for such solutions are also presented.

  10. Scalar Field as a Bose-Einstein Condensate?

    CERN Document Server

    Castellanos, Elías; Núñez, Darío

    2013-01-01

    We present a flat space analogy between a classical scalar field with a self-interacting potential and a Bose-Einstein condensate (BEC). In particular, we reduce the Klein-Gordon equation, governing the dynamics of the scalar field, to a Gross-Pitaevskii--like equation (GPE), governing the dynamics of BEC's. Moreover, the introduction of a curved background spacetime endows, in a natural way, the resulting GPE-like equation with an explicit confinement potential. Additionally, Thomas-Fermi approximation is applied to the 3-dimensional version of this GPE, in order to calculate some thermodynamical properties of the self-interacting scalar field system.

  11. Classical behavior of a scalar field in the inflationary universe

    International Nuclear Information System (INIS)

    Extending the coarse-graining approach of Starobinsky, we formulate a theory to deal with the dynamics of a scalar field in inflationary universe models. We find a set of classical Langevin equations which describes the large scale behavior of the scalar field, provided that the coarse-grained size is greater than the effective compton wavelength of the scalar field. The corresponding Fokker-Planck equation is also derived which is defined on the phase space of the scalar field. We show that our theory is essentially equivalent to the one-loop field theory in de Sitter space and reduces to that of Starobinsky in a strong limit of the slow roll-over condition. Analysis of a simple Higgs potential model is done and the implications are discussed. (author)

  12. Scalar potential without cubic term in 3-3-1 models without exotic electric charges

    Energy Technology Data Exchange (ETDEWEB)

    Giraldo, Yithsbey [Universidad de Narino, Departamento de Fisica, A.A. 1175, Pasto (Colombia); Universidad de Antioquia, Instituto de Fisica, A.A. 1226, Medellin (Colombia); Ponce, William A. [Universidad de Antioquia, Instituto de Fisica, A.A. 1226, Medellin (Colombia)

    2011-07-15

    A detailed study of the criteria for stability of the scalar potential, and the proper electroweak symmetry breaking pattern in some 3-3-1 models without exotic electric charges is presented. In this paper we concentrate in a scalar sector with three Higgs scalar triplets, with a potential that does not include the cubic term, due to the presence of a discrete symmetry. For the analysis we use, and improve, a method previously developed to study the scalar potential in the two-Higgs-doublet extension of the standard model. Our main result is to show the consistency of those 3-3-1 models without exotic electric charges. (orig.)

  13. Role of the scalar field in gravitational lensing

    CERN Document Server

    Virbhadra, K S; Chitre, S M

    1998-01-01

    A static and circularly symmetric lens characterized by mass and scalar charge parameters is constructed. For the small values of the scalar charge to the mass ratio, the gravitational lensing is qualitatively similar to the case of the Schwarzschild lens; however, for large value of this ratio the lensing characteristics are significantly different. The main features are existence of two or nil Einstein ring(s) and a radial critical curve, formation of two or four images and possibility of detecting three images near the lens for sources located at relatively large angular positions. Such a novel lens can also be treated as a naked singularity lens.

  14. Associated single photons and doubly-charged scalars at linear - - colliders

    Indian Academy of Sciences (India)

    Biswarup Mukhopadhyaya; Santosh Kumar Rai

    2007-11-01

    Doubly-charged scalars, predicted in many models having exotic Higgs representations, can in general have lepton-number violating (LFV) couplings. We show that by using an associated monoenergetic final state photon seen at a future linear - - collider, we can have a clear and distinct signature for a doubly-charged resonance. The strength of the = 2 coupling can also be probed quite effectively as a function of the recoil mass of the doubly-charged scalar.

  15. Dwarf galaxies in multistate Scalar Field Dark Matter haloes

    CERN Document Server

    Martinez-Medina, L A; Matos, T

    2014-01-01

    We analyse the velocity dispersion for eight of the Milky Way dwarf spheroidal satellites in the context of finite temperature scalar field dark mater. In this model the finite temperature allows the scalar field to be in configurations that possess excited states, a feature that has proved to be necessary in order to explain the asymptotic rotational velocities found in low surface brightness (LSB) galaxies. In this work we show that excited states are not only important in large galaxies but also have visible effects in dwarf spheroidals. Additionally, we stress that contrary to previous works where the scalar field dark matter haloes are consider to be purely Bose-Einstein condensates, the inclusion of excited states in these halo configurations provides a consistent framework capable of describing LSBs and dwarf galaxies of different sizes without arriving to contradictions within the scalar field dark matter model. Using this new framework we find that the addition of excited states accounts very well fo...

  16. Non-relativistic approach for cosmological Scalar Field Dark Matter

    CERN Document Server

    Urena-Lopez, L Arturo

    2013-01-01

    We derive non-relativistic equations of motion for the formation of cosmological structure in a Scalar Field Dark Matter (SFDM) model corresponding to a complex scalar field endowed with a quadratic scalar potential. Starting with the full equations of motion written in the Newtonian gauge of scalar perturbations, we separate out the fields involved into relativistic and non-relativistic parts, and find the equations of motion for the latter that can be used to build up the full solution. One important assumption will also be that the SFDM field is in the regime of fast oscillations, under which its behavior is exactly that of cold dark matter. The resultant equations are quite similar to the Schr\\"odinger-Poisson system of Newtonian boson stars plus relativistic leftovers. We exploit that similarity to show how to simulate, with minimum numerical effort, the formation of cosmological structure in SFDM models and others alike, and ultimately prove their viability as complete dark matter models.

  17. Noncommutative scalar field minimally coupled to nonsymmetric gravity

    Energy Technology Data Exchange (ETDEWEB)

    Kouadik, S.; Sefai, D. [Laboratory of Mechanic, Physics and Mathematical Modeling Medea University (Algeria)

    2012-06-27

    We construct a non-commutative non symmetric gravity minimally coupled model (the star product only couples matter). We introduce the action for the system considered namely a non-commutative scalar field propagating in a nontrivial gravitational background. We expand the action in powers of the anti-symmetric field and the graviton to second order adopting the assumption that the scalar is weekly coupled to the graviton. We compute the one loop radiative corrections to the self-energy of a scalar particle.

  18. Exact Inflationary Solution to Nonminimally Coupled Scalar Field

    Institute of Scientific and Technical Information of China (English)

    WANG Wen-Fu; YANG Shu-Zheng

    2005-01-01

    @@ We present a new exact inflationary solution to nonminimally coupled scalar field. The inflation is driven by the evolution of scalar field with inflation potential V() = λ/4()4 - 1/2m2()2 + Vo. This includes the solution that behaves exponential inflation for ()o > () > ()end and then develops smoothly towards radiation-like evolution for () < (()end. The spectral index of the scalar density fluctuations, ns, is computed, and the result is consistent with the analysis of the Wilkinson-microwave anisotropy probe data. This model can lead to successful inflation with λ≈ 10-7, rather than 10-13 reported previously.

  19. Cosmological spacetimes balanced by a scale covariant scalar field

    CERN Document Server

    Scholz, Erhard

    2008-01-01

    A scale invariant, Weyl geometric, Lagrangian approach to cosmology is explored, with a a scalar field \\phi of (scale) weight -1 as a crucial ingredient besides classical matter (Tann 1998, Drechsler 1999}. For a particularly simple class of Weyl geometric models (called Einstein-Weyl universes) the Klein-Gordon equation for \\phi is explicitly solvable. In this case the energy-stress tensor of the scalar field consists of a vacuum-like term \\Lambda g_{\\mu \

  20. Quantum reduced loop gravity: Extension to scalar fields

    Science.gov (United States)

    Bilski, Jakub; Alesci, Emanuele; Cianfrani, Francesco

    2015-12-01

    The quantization of the Hamiltonian for a scalar field is performed in the framework of quantum reduced loop gravity. We outline how the regularization can be performed by using the analogous tools adopted in full loop quantum gravity, and the matrix elements of the resulting operator between basis states are analytic coefficients. These achievements open the way for a consistent analysis of the quantum gravity corrections to the classical dynamics of gravity in the presence of a scalar field in a cosmological setting.

  1. Thermal Renormalons in Scalar Field Theory

    CERN Document Server

    Loewe, M

    2000-01-01

    In the frame of the scalar theory $\\lambda \\phi ^{4}$, we explore the occurrence of thermal renormalons, i. e. temperature dependent singularities in the Borel plane. Using Thermofield Dynamics, we found in fact a series of singularities of this kind, which are located to the right of the well known zero temperature pole, being therefore of a subleading character in the ambiguity of the Borel sum.

  2. N-Body Simulations for Coupled Scalar Field Cosmology

    CERN Document Server

    Li, Baojiu

    2010-01-01

    We describe in detail the general methodology and numerical implementation of consistent N-body simulations for coupled scalar field cosmological models, including the background cosmology and the generation of initial conditions (with the different couplings to different matter species taken into account). We perform fully consistent simulations for a class of coupled scalar field models with an inverse power-law potential and negative coupling constant, for which the chameleon mechanism does not operate. We find that in such cosmological models the scalar-field potential plays a negligible role except in the background expansion, and the fifth force that is produced is proportional to gravity in magnitude, justifying the use of a rescaled gravitational constant G in some earlier N-body simulations of similar models. We study the effects of the scalar coupling on the nonlinear matter power spectra and compare with linear perturbation calculations to investigate where the nonlinear model deviates from the lin...

  3. Quark scalar, axial, and pseudoscalar charges in the Schwinger-Dyson formalism

    OpenAIRE

    Yamanaka, Nodoka; Imai, Shotaro; Doi, Takahiro M.; Suganuma, Hideo

    2014-01-01

    We calculate the scalar, axial, and pseudoscalar charges of the quark in the Schwinger-Dyson formalism of Landau gauge QCD. It is found that the dressed quark scalar density of the valence quark is significantly enhanced against the bare quark contribution, and the result explains qualitatively the phenomenologically known value of the pion-nucleon sigma term and also that given by lattice QCD. Moreover, we show that the Richardson's interquark potential suppresses the quark scalar density in...

  4. Gauge Fields and Scalars in Rolling Tachyon Backgrounds

    OpenAIRE

    Mehen, Thomas; Wecht, Brian

    2002-01-01

    We investigate the dynamics of gauge and scalar fields on unstable D-branes with rolling tachyons. Assuming an FRW metric on the brane, we find a solution of the tachyon equation of motion which is valid for arbitrary tachyon potentials and scale factors. The equations of motion for a U(1) gauge field and a scalar field in this background are derived. These fields see an effective metric which differs from the original FRW metric. The field equations receive large corrections due to the curva...

  5. Building a Holographic Superconductor with a Scalar Field Coupled Kinematically to Einstein Tensor

    CERN Document Server

    Kuang, Xiao-Mei

    2016-01-01

    We study the holographic dual description of a superconductor in which the gravity sector consists of a Maxwell field and a charged scalar field which except its minimal coupling to gravity it is also coupled kinematically to Einstein tensor. As the strength of the new coupling is increased, the critical temperature below which the scalar field condenses is lowering, the condensation gap decreases faster than the temperature, the width of the condensation gap is not proportional to the size of the condensate and at low temperatures the condensation gap tends to zero for the strong coupling. These effects which are the result of the presence of the coupling of the scalar field to the Einstein tensor in the gravity bulk, provide a dual description of impurities concentration in a superconducting state on the boundary.

  6. Generalized cosmic Chaplygin gas inspired intermediate standard scalar field inflation

    Science.gov (United States)

    Jawad, Abdul; Rani, Shamaila; Mohsaneen, Sidra

    2016-08-01

    We study the warm intermediate inflationary regime in the presence of generalized cosmic Chaplygin gas and an inflaton decay rate proportional to the temperature. For this purpose, we consider standard scalar field model during weak and strong dissipative regimes. We explore inflationary parameters like spectral index, scalar and tensor power spectra, tensor to scalar ratio and decay rate in order to compare the present model with recent observational data. The physical behavior of inflationary parameters is presented and found that all the results are agreed with recent observational data such as WMAP7, WMAP9 and Planck 2015.

  7. The self-force on a non-minimally coupled static scalar charge outside a Schwarzschild black hole

    Energy Technology Data Exchange (ETDEWEB)

    Cho, Demian H J; Tsokaros, Antonios A; Wiseman, Alan G [Department of Physics, University of Wisconsin-Milwaukee, PO Box 413, Milwaukee, WI 53201 (United States)

    2007-03-07

    The finite part of the self-force on a static, non-minimally coupled scalar test charge outside a Schwarzschild black hole is zero. This result is determined from the work required to slowly raise or lower the charge through an infinitesimal distance. Unlike similar force calculations for minimally-coupled scalar charges or electric charges, we find that we must account for a flux of field energy that passes through the horizon and changes the mass and area of the black hole when the charge is displaced. This occurs even for an arbitrarily slow displacement of the non-minimally coupled scalar charge. For a positive coupling constant, the area of the hole increases when the charge is lowered and decreases when the charge is raised. The fact that the self-force vanishes for a static, non-minimally coupled scalar charge in Schwarzschild spacetime agrees with a simple prediction of the Quinn-Wald axioms. However, Zel'nikov and Frolov computed a non-vanishing self-force for a non-minimally coupled charge. Our method of calculation closely parallels the derivation of Zel'nikov and Frolov, and we show that their omission of this unusual flux is responsible for their (incorrect) result. When the flux is accounted for, the self-force vanishes. This correction eliminates a potential counter example to the Quinn-Wald axioms. The fact that the area of the black hole changes when the charge is displaced brings up two interesting questions that did not arise in similar calculations for static electric charges and minimally coupled scalar charges. (1) How can we reconcile a decrease in the area of the black hole horizon with the area theorem which concludes that {delta}Area{sub horizon} {>=} 0? The key hypothesis of the area theorem is that the stress-energy tensor must satisfy a null-energy condition T{sup {alpha}}{sup {beta}}l{sub {alpha}}l{sub {beta}} {>=} 0 for any null vector l{sub {alpha}}. We explicitly show that the stress-energy associated with a non

  8. Cosmic string interactions induced by gauge and scalar fields

    CERN Document Server

    Kabat, Daniel

    2012-01-01

    We study the interaction between two parallel cosmic strings induced by gauge fields and by scalar fields with non-minimal couplings to curvature. For small deficit angles the gauge field behaves like a collection of non-minimal scalars with a specific value for the non-minimal coupling. We check this equivalence by computing the interaction energy between strings at first order in the deficit angles. This result provides another physical context for the "contact terms" which play an important role in the renormalization of black hole entropy due to a spin-1 field.

  9. Thermodynamics of perfect fluids from scalar field theory

    Science.gov (United States)

    Ballesteros, Guillermo; Comelli, Denis; Pilo, Luigi

    2016-07-01

    The low-energy dynamics of relativistic continuous media is given by a shift-symmetric effective theory of four scalar fields. These scalars describe the embedding in spacetime of the medium and play the role of Stückelberg fields for spontaneously broken spatial and time translations. Perfect fluids are selected imposing a stronger symmetry group or reducing the field content to a single scalar. We explore the relation between the field theory description of perfect fluids to thermodynamics. By drawing the correspondence between the allowed operators at leading order in derivatives and the thermodynamic variables, we find that a complete thermodynamic picture requires the four Stückelberg fields. We show that thermodynamic stability plus the null-energy condition imply dynamical stability. We also argue that a consistent thermodynamic interpretation is not possible if any of the shift symmetries is explicitly broken.

  10. Higgs and gravitational scalar fields together induce Weyl gauge

    Science.gov (United States)

    Scholz, Erhard

    2015-02-01

    A common biquadratic potential for the Higgs field and an additional scalar field , non minimally coupled to gravity, is considered in a locally scale symmetric approach to standard model fields in curved spacetime. A common ground state of the two scalar fields exists and couples both fields to gravity, more precisely to Weyl geometric scalar curvature . In Einstein gauge (, often called "Einstein frame"), also is scaled to a constant. This condition makes perfect sense, even in the general case, in the Weyl geometric approach. There it has been called Weyl gauge, because it was first considered by Weyl in the different context of his original scale geometric theory of gravity of 1918. Now it may get new meaning as a combined effect of electroweak theory and gravity, and their common influence on atomic frequencies.

  11. Higgs and gravitational scalar fields together induce Weyl gauge

    CERN Document Server

    Scholz, Erhard

    2014-01-01

    A common biquadratic potential for the Higgs field $h$ and an additional scalar field $\\phi$, non minimally coupled to gravity, is considered in locally scale symmetric approaches to standard model fields in curved spacetime. A common ground state of the two scalar fields exists and couples both fields to gravity, more precisely to scalar curvature $R$. In Einstein gauge ($\\phi = const$, often called "Einstein frame"), also $R$ is scaled to a constant. This condition makes perfect sense, even in the general case, in the Weyl geometric approach. There it has been called {\\em Weyl gauge}, because it was first considered by Weyl in the different context of his original scale geometric theory of gravity of 1918. Now it seems to get new meaning as a combined effect of electroweak theory and gravity, and their common influence on atomic frequencies.

  12. Thermodynamics of perfect fluids from scalar field theory

    CERN Document Server

    Ballesteros, Guillermo; Pilo, Luigi

    2016-01-01

    The low-energy dynamics of relativistic continuous media is given by a shift-symmetric effective theory of four scalar fields. These scalars describe the embedding in spacetime of the medium and play the role of Stuckelberg fields for spontaneously broken spatial and time translations. Perfect fluids are selected imposing a stronger symmetry group or reducing the field content to a single scalar. We explore the relation between the field theory description of perfect fluids to thermodynamics. By drawing the correspondence between the allowed operators at leading order in derivatives and the thermodynamic variables, we find that a complete thermodynamic picture requires the four Stuckelberg fields. We show that thermodynamic stability plus the null energy condition imply dynamical stability. We also argue that a consistent thermodynamic interpretation is not possible if any of the shift symmetries is explicitly broken.

  13. Time evolutions of scalar field perturbations in $D$-dimensional Reissner-Nordstr\\"om Anti-de Sitter black holes

    CERN Document Server

    Li, Ran; Zhao, Junkun

    2016-01-01

    Reissner-Nordstr\\"om Anti-de Sitter (RNAdS) black holes are unstable against the charged scalar field perturbations due to the well-known superradiance phenomenon. We present the time domain analysis of charged scalar field perturbations in the RNAdS black hole background in general dimensions. We show that the instabilities of charged scalar field can be explicitly illustrated from the time profiles of evolving scalar field. By using the Prony method to fit the time evolution data, we confirm the mode that dominates the long time behavior of scalar field is in accordance with the quasinormal mode from the frequency domain analysis. The superradiance origin of the instability can also be demonstrated by comparing the real part of the dominant mode with the superradiant condition of charged scalar field. It is shown that all the unstable modes are superradiant, which is consistent with the analytical result in the frequency domain analysis. Furthermore, we also confirm there exists the rapid exponential growin...

  14. A Riccati equation based approach to isotropic scalar field cosmologies

    Science.gov (United States)

    Harko, Tiberiu; Lobo, Francisco S. N.; Mak, M. K.

    2014-05-01

    Gravitationally coupled scalar fields ϕ, distinguished by the choice of an effective self-interaction potential V(ϕ), simulating a temporarily nonvanishing cosmological term, can generate both inflation and late time acceleration. In scalar field cosmological models the evolution of the Hubble function is determined, in terms of the interaction potential, by a Riccati type equation. In the present work, we investigate scalar field cosmological models that can be obtained as solutions of the Riccati evolution equation for the Hubble function. Four exact integrability cases of the field equations are presented, representing classes of general solutions of the Riccati evolution equation. The solutions correspond to cosmological models in which the Hubble function is proportional to the scalar field potential plus a linearly decreasing function of time, models with the time variation of the scalar field potential proportional to the potential minus its square, models in which the potential is the sum of an arbitrary function and the square of the function integral, and models in which the potential is the sum of an arbitrary function and the derivative of its square root, respectively. The cosmological properties of all models are investigated in detail, and it is shown that they can describe the inflationary or the late accelerating phase in the evolution of the universe.

  15. Note on scalars, perfect fluids, constrained field theories, and all that

    CERN Document Server

    Diez-Tejedor, Alberto

    2013-01-01

    The relation of a scalar field with a perfect fluid has generated some debate along the last few years. In this paper we argue that shift-invariant scalar fields can describe accurately the potential flow of an isentropic perfect fluid, but, in general, the identification is possible only for a finite period of time. After that period in the evolution the dynamics of the scalar field and the perfect fluid branch off. The Lagrangian density for the velocity-potential can be read directly from the expression relating the pressure with the Taub charge and the entropy per particle in the fluid, whereas the other quantities of interest can be obtained from the thermodynamic relations.

  16. Quantum and classical aspects of scalar and vector fields around black holes

    CERN Document Server

    Wang, Mengjie

    2016-01-01

    This thesis presents recent studies on test scalar and vector fields around black holes. It is separated in two parts according to the asymptotic properties of the spacetime under study. In the first part, we investigate scalar and Proca fields on an asymptotically flat background. For the Proca field, we obtain a complete set of equations of motion in higher dimensional spherically symmetric backgrounds. These equations are solved numerically, both to compute Hawking radiation spectra and quasi-bound states. In the former case, we carry out a precise study of the longitudinal degrees of freedom induced by the field mass. This can be used to improve the model in the black hole event generators currently used at the Large Hadron Collider. Regarding quasi-bound states, we find arbitrarily long lived modes for a charged Proca field, as well as for a charged scalar field, in a Reissner-Nordstr\\"om black hole. The second part of this thesis presents research on superradiant instabilities of scalar and Maxwell fiel...

  17. Higgs portal dark matter and neutrino mass and mixing with a doubly charged scalar

    CERN Document Server

    Hierro, I M; Rigolin, S

    2016-01-01

    We consider an extension of the Standard Model involving two new scalar particles around the TeV scale: a singlet neutral scalar $\\phi$, to be eventually identified as the Dark Matter candidate, plus a doubly charged $SU(2)_L$ singlet scalar, $S^{++}$, that can be the source for the non-vanishing neutrino masses and mixings. Assuming an unbroken $Z_2$ symmetry in the scalar sector, under which only the additional neutral scalar $\\phi$ is odd, we write the most general (renormalizable) scalar potential. The model may be regarded as a possible extension of the conventional Higgs portal Dark Matter scenario which also accounts for neutrino mass and mixing. This framework cannot completely explain the observed positron excess. However a softening of the discrepancy observed in conventional Higgs portal framework can be obtained, especially when the scale of new physics responsible for generating neutrino masses and lepton number violating processes is around 2 TeV.

  18. Quasistationary solutions of scalar fields around accreting black holes

    Science.gov (United States)

    Sanchis-Gual, Nicolas; Degollado, Juan Carlos; Izquierdo, Paula; Font, José A.; Montero, Pedro J.

    2016-08-01

    Massive scalar fields can form long-lived configurations around black holes. These configurations, dubbed quasibound states, have been studied both in the linear and nonlinear regimes. In this paper, we show that quasibound states can form in a dynamical scenario in which the mass of the black hole grows significantly due to the capture of infalling matter. We solve the Klein-Gordon equation numerically in spherical symmetry, mimicking the evolution of the spacetime through a sequence of analytic Schwarzschild black hole solutions of increasing mass. It is found that the frequency of oscillation of the quasibound states decreases as the mass of the black hole increases. In addition, accretion leads to an increase of the exponential decay of the scalar field energy. We compare the black hole mass growth rates used in our study with estimates from observational surveys and extrapolate our results to values of the scalar field masses consistent with models that propose scalar fields as dark matter in the universe. We show that, even for unrealistically large mass accretion rates, quasibound states around accreting black holes can survive for cosmological time scales. Our results provide further support to the intriguing possibility of the existence of dark matter halos based on (ultralight) scalar fields surrounding supermassive black holes in galactic centers.

  19. Effective Action for Cosmological Scalar Fields at Finite Temperature

    CERN Document Server

    Cheung, Yeuk-Kwan E; Kang, Jin U; Kim, Jong Chol

    2015-01-01

    Scalar fields appear in many theories beyond the Standard Model of particle physics. In the early universe, they are exposed to extreme conditions, including high temperature and rapid cosmic expansion. Understanding their behavior in this environment is crucial to understand the implications for cosmology. We calculate the finite temperature effective action for the field expectation value in two particularly important cases, for damped oscillations near the ground state and for scalar fields with a flat potential. We find that the behavior in both cases can in good approximation be described by a complex valued effective potential that yields Markovian equations of motion. Near the potential minimum, we recover the solution to the well-known Langevin equation. For large field values we find a very different behavior, and our result for the damping coefficient significantly differs from the expressions given in the literature. We illustrate our results in a simple scalar model, for which we give analytic app...

  20. Small scale structures in coupled scalar field dark matter

    Directory of Open Access Journals (Sweden)

    J. Beyer

    2014-11-01

    Full Text Available We investigate structure formation for ultra-light scalar field dark matter coupled to quintessence, in particular the cosmon–bolon system. The linear power spectrum is computed by a numerical solution of the coupled field equations. We infer the substructure abundance within a Milky Way-like halo. Estimates of dark halo abundances from recent galaxy surveys imply a lower bound on the bolon mass of about 9×10−22 eV. This seems to exclude a possible detection of scalar field dark matter through time variation in pulsar timing signals in the near future.

  1. Primordial magnetic fields from self-ordering scalar fields

    CERN Document Server

    Horiguchi, Kouichirou; Sekiguchi, Toyokazu; Sugiyama, Naoshi

    2015-01-01

    A symmetry-breaking phase transition in the early universe could have led to the formation of cosmic defects. Because these defects dynamically excite not only scalar and tensor type cosmological perturbations but also vector type ones, they may serve as a source of primordial magnetic fields. In this study, we calculate the time evolution and the spectrum of magnetic fields that are generated by a type of cosmic defects, called global textures, using the non-linear sigma (NLSM) model. Based on the standard cosmological perturbation theory, we show, both analytically and numerically, that a vector-mode relative velocity between photon and baryon fluids is induced by textures, which inevitably leads to the generation of magnetic fields over a wide range of scales. We find that the amplitude of the magnetic fields is given by $B\\sim{10^{-9}}{((1+z)/10^3)^{-2.5}}({v}/{m_{\\rm pl}})^2({k}/{\\rm Mpc^{-1}})^{3.5}/{\\sqrt{N}}$ Gauss in the radiation dominated era for $k\\lesssim 1$ Mpc$^{-1}$, with $v$ being the vacuum ...

  2. Direct Reconstruction of the Dark Energy Scalar-Field Potential

    CERN Document Server

    Li, C; Cooray, A R; Li, Chao; Holz, Daniel E.; Cooray, Asantha

    2006-01-01

    While the accelerated expansion of the Universe is by now well established, an underlying scalar field potential possibly responsible for this acceleration remains unconstrained. We present an attempt to reconstruct this potential using recent SN data, under the assumption that the acceleration is driven by a single scalar field. Current approaches to such reconstructions are based upon simple parametric descriptions of either the luminosity distance or the dark energy equation of state. We find that these various approximations lead to different derived evolutionary histories of the dark energy equation of state (although there is considerable overlap between the different potential shapes allowed by the data). Depending upon one's assumptions, the same SN data set can lead to divergent statements about properties of the dark energy. Instead of these indirect reconstruction schemes, we discuss a technique to determine the potential directly from the data by expressing it in terms of a binned scalar field. In...

  3. Behavior of Phantom Scalar Fields near Black Holes

    CERN Document Server

    Lora-Clavijo, F D; Guzman, F S; 10.1063/1.3473875

    2012-01-01

    We present the accretion of a phantom scalar field into a black hole for various scalar field potentials in the full non-linear regime. Our results are based on the use of numerical methods and show that for all the cases studied the black hole's apparent horizon mass decreases. We explore a particular subset of the parameter space and from our results we conclude that this is a very efficient black hole shrinking process because the time scales of the area reduction of the horizon are short. We show that the radial equation of state of the scalar field depends strongly on the space and time, with the condition $\\omega = p/\\rho>-1$, as opposed to a phantom fluid at cosmic scales that allows $\\omega < -1$.

  4. Loop quantum gravity coupled to a scalar field

    Science.gov (United States)

    Lewandowski, Jerzy; Sahlmann, Hanno

    2016-01-01

    We consider the model of gravity coupled to the Klein-Gordon time field. We do not deparametrize the theory using the scalar field before quantization, but quantize all degrees of freedom. Several new results for loop quantum gravity are obtained: (i) a Hilbert space for the gravity-matter system and a nonstandard representation of the scalar field thereon is constructed, (ii) a new operator for the scalar constraint of the coupled system is defined and investigated, (iii) methods for solving the constraint are developed. Commutators of the new quantum constraint operators correspond to the quantization of the Poisson bracket. This, however, poses problems for finding solutions. Hence the states we consider—and perhaps the whole setup—still needs some improvement. As a side result we describe a representation of the gravitational degrees of freedom in which the flux is diagonal. This representation is related to the BF theory vacuum of Dittrich and Geiller.

  5. Bose–Einstein condensates and scalar fields; exploring the similitudes

    Energy Technology Data Exchange (ETDEWEB)

    Castellanos, E. [Departamento de Física, Centro de Investigación y de Estudios Avanzados del IPN, A.P. 14-740, 07000 México D.F. (Mexico); Macías, A. [Departamento de Física, Universidad Autónoma Metropolitana-Iztapalapa, A.P. 55-534, México D.F. 09340 (Mexico); Núñez, D. [Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior C.U., A.P. 70-543, México D.F. 04510 (Mexico)

    2014-01-14

    We analyze the the remarkable analogy between the classical Klein–Gordon equation for a test scalar field in a flat and also in a curved background, and the Gross–Pitaevskii equation for a Bose–Einstein condensate trapped by an external potential. We stress here that the solution associated with the Klein–Gordon equation (KG) in a flat space time has the same mathematical structure, under certain circumstances, to those obtained for the Gross–Pitaevskii equation, that is, a static soliton solution. Additionally, Thomas–Fermi approximation is applied to the 3–dimensional version of this equation, in order to calculate some thermodynamical properties of the system in curved a space–time back ground. Finally, we stress the fact that a gravitational background provides, in some cases, a kind of confining potential for the scalar field, allowing us to remarks even more the possible connection between scalar fields and the phenomenon of Bose–Einstein condensation.

  6. Boson Stars in a Theory of Complex Scalar Field coupled to Gravity

    CERN Document Server

    Kumar, Sanjeev; Kulshreshtha, Daya Shankar

    2016-01-01

    We study boson stars in a theory of complex scalar field coupled to Einstein gravity with the potential: $V(|\\Phi|) := m^{2} |\\Phi|^2 +2 \\lambda |\\Phi|$ (where $m^2$ and $\\lambda$ are positive constant parameters). This could be considered either as a theory of massive complex scalar field coupled to gravity in a conical potential or as a theory in the presence of a potential which is an overlap of a parabolic and a conical potential. We study our theory with positive as well as negative values of the cosmological constant $\\Lambda$. Boson stars are found to come in two types, having either ball-like or shell-like charge density. We have studied the properties of these solutions and have also determined their domains of existence for some specific values of the parameters of the theory. Similar solutions have also been obtained by Hartmann, Kleihaus, Kunz, and Schaffer, in a V-shaped scalar potential.

  7. Irreducible Cartesian tensor expansions of scalar fields

    International Nuclear Information System (INIS)

    It is shown how a scalar function V(parallel R + Σ/sub i equals 1/sup n/ a/sub i/parallel) of a sum of n + 1 vectors can be expanded as a multiple Cartesian tensor series in the vectors a/ sub i/. This expansion is a rearrangement of the multiple Taylor series expansion of such a function. In order to prove the fundamental theorem, generalized Cartesian Legendre polynomials are defined. The theorem is applied to the eigenfunctions of the Laplace operator and to inverse powers. The expansion of the latter type of function leads to forms involving generalized hypergeometric functions in several variables. As a special case, the Cartesian form of the multipole expansion of the electrostatic potential between two linear molecules is derived. A number of sum rules for hypergeometric functions and addition formulas for (standard and modified) spherical Bessel functions are proved by using a reduction property of the generalized Legendre polynomials. The case of the expansion of a tensorial function is also briefly discussed

  8. Homogenization Theory for a Replenishing Passive Scalar Field

    Institute of Scientific and Technical Information of China (English)

    Peter R.KRAMER; Shane R.KEATING

    2009-01-01

    Homogenization theory provides a rigorous framework for calculating the effective diffusivity of a decaying passive scalar field in a turbulent or complex flow.The authors extend this framework to the case where the passive scalar fluctuations ore continuously replenished by a source(and/or sink).The basic structure.of the homogenized equations carries over,but in some eases the homogenized source can involve a non-trivial coupling of the velocity field and the source.The authors derive expressions for the homogenized source term for various multiscale source structures and interpret them physically.

  9. Cosmological spacetimes balanced by a scale covariant scalar field

    OpenAIRE

    Scholz, Erhard

    2008-01-01

    A scale invariant, Weyl geometric, Lagrangian approach to cosmology is explored, with a a scalar field phi of (scale) weight -1 as a crucial ingredient besides classical matter \\cite{Tann:Diss,Drechsler:Higgs}. For a particularly simple class of Weyl geometric models (called {\\em Einstein-Weyl universes}) the Klein-Gordon equation for phi is explicitly solvable. In this case the energy-stress tensor of the scalar field consists of a vacuum-like term Lambda g_{mu nu} with variable coefficient ...

  10. Langevin description of gauged scalar fields in a thermal bath

    CERN Document Server

    Miyamoto, Yuhei; Suyama, Teruaki; Yokoyama, Jun'ichi

    2013-01-01

    We study the dynamics of the oscillating gauged scalar field in a thermal bath. A Langevin type equation of motion of the scalar field, which contains both dissipation and fluctuation terms, is derived by using the real-time finite temperature effective action approach. The existence of the quantum fluctuation-dissipation relation between the non-local dissipation term and the Gaussian stochastic noise terms is verified. We find the noise variables are anti-correlated at equal-time. The dissipation rate for the each mode is also studied, which turns out to depend on the wavenumber.

  11. Braneworld inflation with a complex scalar field from Planck 2015

    Science.gov (United States)

    Mounzi, Z.; Ferricha-Alami, M.; Chakir, H.; Bennai, M.

    2016-06-01

    We study an inflationary model with a single complex scalar field in the framework of braneworld Randall-Sundrum model type 2. From the scalar curvature perturbation constrained by the recent observation values, and for specific choice of parameters, we can reduce the values of the coupling constant to take the natural values, and we found that the phase theta θ of the inflation field can take the narrow interval. We have also derived all known inflationary parameters (ns, r and dns/d ln (k)), which are widely consistent with the recent Planck data for a suitable choice of brane tension value λ.

  12. On static solutions of the Einstein - Scalar Field equations

    CERN Document Server

    Reiris, Martin

    2015-01-01

    In this note we study the Einstein-ScalarField static equations in arbitrary dimensions. We discuss the existence of geodesically complete solutions depending on the form of the scalar field potential $V(\\phi)$, and provide full global geometric estimates when the solutions exist. As a special case it is shown that when $V(\\phi)$ is the Klein-Gordon potential, i.e. $V(\\phi)=m^{2}|\\phi|^{2}$, geodesically complete solutions are necessarily Ricci-flat, have constant lapse and are vacuum, (that is $\\phi=\\phi_{0}$ with $\\phi_{0}=0$ if $m\

  13. Dynamical Analysis of Scalar Field Cosmologies with Spatial Curvature

    CERN Document Server

    Gosenca, Mateja

    2015-01-01

    We explore the dynamical behaviour of cosmological models involving a scalar field (with an exponential potential and a canonical kinetic term) and a matter fluid with spatial curvature included in the equations of motion. Using appropriately defined parameters to describe the evolution of the scalar field energy in this situation, we find that there are two extra fixed points that are not present in the case without curvature. We also analyse the evolution of the effective equation-of-state parameter for different initial values of the curvature.

  14. Observational Constraints on New Exact Inflationary Scalar-field Solutions

    CERN Document Server

    Barrow, John D

    2016-01-01

    An algorithm is used to generate new solutions of the scalar field equations in homogeneous and isotropic universes. Solutions can be found for pure scalar fields with various potentials in the absence and presence of spatial curvature and other perfect fluids. A series of generalisations of the Chaplygin gas and bulk viscous cosmological solutions for inflationary universes are found. We also show how the Hubble slow-roll parameters can be calculated using the solution algorithm and we compare these inflationary solutions with the observational data provided by the Planck 2015 collaboration in order to constraint and rule out some of these models.

  15. Effective field theory of modified gravity with two scalar fields: dark energy and dark matter

    OpenAIRE

    Gergely, László Á.; Tsujikawa, Shinji

    2014-01-01

    We present a framework for discussing the cosmology of dark energy and dark matter based on two scalar degrees of freedom. An effective field theory of cosmological perturbations is employed. A unitary gauge choice renders the dark energy field into the gravitational sector, for which we adopt a generic Lagrangian depending on three-dimensional geometrical scalar quantities arising in the ADM decomposition. We add to this dark-energy associated gravitational sector a scalar field $\\phi$ and i...

  16. Effective action for scalar fields in two-dimensional gravity

    International Nuclear Information System (INIS)

    We consider a general two-dimensional gravity model minimally or nonminimally coupled to a scalar field. The canonical form of the model is elucidated, and a general solution of the equations of motion in the massless case is reviewed. In the presence of a scalar field all geometric fields (zweibein and Lorentz connection) are excluded from the model by solving exactly their Hamiltonian equations of motion. In this way the effective equations of motion and the corresponding effective action for a scalar field are obtained. It is written in a Minkowskian space-time and does not include any geometric variables. The effective action arises as a boundary term and is nontrivial both for open and closed universes. The reason is that unphysical degrees of freedom cannot be compactly supported because they must satisfy the constraint equation. As an example we consider spherically reduced gravity minimally coupled to a massless scalar field. The effective action is used to reproduce the Fisher and Roberts solutions

  17. Conformal Field Theory Correlators from Classical Scalar Field Theory on $AdS_{d+1}$

    CERN Document Server

    Mück, W; Mueck, Wolfgang

    1998-01-01

    We use the correspondence between scalar field theory on $AdS_{d+1}$ and a conformal field theory on $R^d$ to calculate the 3- and 4-point functions of the latter. The classical scalar field theory action is evaluated at tree level.

  18. Weak Gravitational Wave and Casimir Energy of a Scalar Field

    Science.gov (United States)

    Tavakoli, F.; Pirmoradian, R.; Parsabod, I.

    2016-09-01

    In this paper, we calculate the effect of a weak gravitational field on the Casimir force between two ideal plates subjected to a massless minimally coupled field. It is the aim of this work to study the Casimir energy under a weak perturbation of gravity. Moreover, the fluctuations of the stress-energy tensor for a scalar field in de Sitter space-time are computed as well.

  19. Scalar field theory on fuzzy S{sup 4}

    Energy Technology Data Exchange (ETDEWEB)

    Medina, Julieta; O' Connor, Denjoe [School of Theoretical Physics, Dublin Institute for Advanced Studies, Dublin (Ireland) and Depto de Fisica, Cinvestav, Mexico (Mexico)]. E-mail addresses: julieta@stp.dias.ie, denjoe@stp.dias.ie

    2003-11-01

    Scalar fields are studied on fuzzy S{sup 4} and a solution is found for the elimination of the unwanted degrees of freedom that occur in the model. The resulting theory can be interpreted as a Kaluza-Klein reduction of CP{sup 3} to S{sup 4} in the fuzzy context. (author)

  20. Dwarf galaxies in multistate scalar field dark matter halos

    Science.gov (United States)

    Martinez-Medina, L. A.; Robles, V. H.; Matos, T.

    2015-01-01

    We analyze the velocity dispersion for eight of the Milky Way dwarf spheroidal satellites in the context of finite temperature scalar field dark matter. In this model the finite temperature allows the scalar field to be in configurations that possess excited states, a feature that has proved to be necessary in order to explain the asymptotic rotational velocities found in low surface brightness (LSB) galaxies. In this work we show that excited states are not only important in large galaxies but also have visible effects in dwarf spheroidals. Additionally, we stress that contrary to previous works where the scalar field dark matter halos are consider to be purely Bose-Einstein condensates, the inclusion of excited states in these halo configurations provides a consistent framework capable of describing LSB and dwarf galaxies of different sizes without arriving to contradictions within the scalar field dark matter model. Using this new framework we find that the addition of excited states accounts very well for the raise in the velocity dispersion in Milky Way dwarf spheroidal galaxies improving the fit compared to the one obtained assuming all the dark matter to be in the form of a Bose-Einstein condensate.

  1. Effective action for a quantum scalar field in warped spaces

    Energy Technology Data Exchange (ETDEWEB)

    Hoff da Silva, J.M.; Mendonca, E.L.; Scatena, E. [Universidade Estadual Paulista ' ' Julio de Mesquita Filho' ' -UNESP, Departamento de Fisica e Quimica, Guaratingueta, SP (Brazil)

    2015-11-15

    We investigate the one-loop corrections, at zero as well as finite temperature, of a scalar field taking place in a braneworld motivated warped background. After to reach a well-defined problem, we calculate the effective action with the corresponding quantum corrections to each case. (orig.)

  2. Scalar field entanglement entropy for small Schwarzschild black hole

    OpenAIRE

    Teslyk, Maksym; Teslyk, Olena

    2013-01-01

    We consider scalar field entanglement entropy generated with black hole of (sub)planck mass scale thus implying the unitary evolution of gravity. The dependence on the dimension of the Hilbert space for degrees of freedom located behind the horizon is taken into account. The obtained results contain polylogarithmic terms.

  3. Scalar fields in the late Universe: The mechanical approach

    CERN Document Server

    Burgazli, Alvina; Morais, João; Kumar, K Sravan

    2015-01-01

    In this paper, we consider the Universe at the late stage of its evolution and deep inside the cell of uniformity. At these scales, we consider the Universe to be filled with dust-like matter in the form of discretely distributed galaxies, a minimal scalar field, the cosmological constant and radiation as matter sources. We investigate such a Universe in the mechanical approach. This means that the peculiar velocities of the inhomogeneities (in the form of galaxies) as well as fluctuations of other perfect fluids are non-relativistic. Under such conditions, we investigate the theory of scalar perturbations. We show that, at the background level, the considered scalar field has a constant equation of state (EoS) parameter $w=-1/3$. The fluctuations of the energy density and pressure of this field are defined by the interaction between scalar field background and the gravitational potential of the system. These fluctuations are concentrated around the galaxies screening their gravitational potentials. The expre...

  4. Brane Structure from Scalar Field in Warped Spacetime

    CERN Document Server

    Bazeia, D; Gomes, A R

    2004-01-01

    We deal with scalar field coupled to gravity in five dimensions in warped geometry. We investigate models described by potentials that drive the system to support thick brane solutions that engender internal structure. We also show that the brane solutions simulate the occurrence of the complete wetting phenomenon at high temperatures.

  5. A variational approach to homogeneous scalar fields in General Relativity

    CERN Document Server

    Giambo', R; Magli, G

    2006-01-01

    A result of existence of homogeneous scalar field solutions between prescribed configurations is given, using a modified version of Euler--Maupertuis least action variational principle. Solutions are obtained as limit of approximating variational problems, solved using techniques introduced by Rabinowitz.

  6. Higgs particles interacting via a scalar Dark Matter field

    Science.gov (United States)

    Bhattacharya, Yajnavalkya; Darewych, Jurij

    2016-07-01

    We study a system of two Higgs particles, interacting via a scalar Dark Matter mediating field. The variational method in the Hamiltonian formalism of QFT is used to derive relativistic wave equations for the two-Higgs system, using a truncated Fock-space trial state. Approximate solutions of the two-body equations are used to examine the existence of Higgs bound states.

  7. Effects of a scalar scaling field on quantum mechanics

    Science.gov (United States)

    Benioff, Paul

    2016-07-01

    This paper describes the effects of a complex scalar scaling field on quantum mechanics. The field origin is an extension of the gauge freedom for basis choice in gauge theories to the underlying scalar field. The extension is based on the idea that the value of a number at one space time point does not determine the value at another point. This, combined with the description of mathematical systems as structures of different types, results in the presence of separate number fields and vector spaces as structures, at different space time locations. Complex number structures and vector spaces at each location are scaled by a complex space time dependent scaling factor. The effect of this scaling factor on several physical and geometric quantities has been described in other work. Here the emphasis is on quantum mechanics of one and two particles, their states and properties. Multiparticle states are also briefly described. The effect shows as a complex, nonunitary, scalar field connection on a fiber bundle description of nonrelativistic quantum mechanics. The lack of physical evidence for the presence of this field so far means that the coupling constant of this field to fermions is very small. It also means that the gradient of the field must be very small in a local region of cosmological space and time. Outside this region, there are no restrictions on the field gradient.

  8. Exact Inflationary Solution in String-Motivated Scalar Field Cosmology

    Institute of Scientific and Technical Information of China (English)

    王文福

    2001-01-01

    We present a new exact solution to Einstein's equations that describes the evolution of inflationary universe models. The inflation is driven by the evolution of a scalar field with an approximate two-loop four-dimensional string potential. In this scenario, the inflation began immediately after the epoch governed by quantum gravity and therefore there is no initial singularity. The successful inflation scenario is expected to appear only at two loop order. For a1/|a2| ≥ 90, the spectral index ns of the scalar density fluctuations lies well inside the limits set by the cosmic background explorer satellite and the gravitational wave spectral index is ng≈1.

  9. Scalar self-force on a static particle in Schwarzschild using the massive field approach

    OpenAIRE

    Rosenthal, Eran

    2004-01-01

    We use the recently developed massive field approach to calculate the scalar self-force on a static particle in a Schwarzschild spacetime. In this approach the scalar self-force is obtained from the difference between the (massless) scalar field, and an auxiliary massive scalar field combined with a certain limiting process. By applying this approach to a static particle in Schwarzschild we show that the scalar self-force vanishes in this case. This result conforms with a previous analysis by...

  10. Multi high charged scalars in the LHC searches and Majorana neutrino mass generations

    CERN Document Server

    Chen, Chian-Shu; Tsai, Lu-Hsing

    2013-01-01

    Motivated by the large rate of $H\\to \\gamma\\gamma$ at the LHC, we explore a class of models with high dimensional representations of scalars to realize small Majorana neutrino masses at two-loop level without imposing any new symmetry. In these models, multi scalars with the electric charges higher than two are naturally expected, which not only enhance the $H\\to \\gamma\\gamma$ rate, but provide more searching grounds at the LHC.

  11. Tunnelling of scalar and Dirac particles from squashed charged rotating Kaluza-Klein black holes

    CERN Document Server

    Stetsko, M M

    2014-01-01

    Thermal radiation of scalar particles and Dirac fermions from squashed charged rotating five-dimensional black holes is considered. To obtain temperature of the black holes we use the tunnelling method. In case of scalar particles we make use of the Hamilton-Jacobi equation. To consider tunnelling of fermions the Dirac equation was investigated. The examination shows that radial parts of the action for scalar particles and fermions in quasi-classical limit in the vicinity of horizon are almost the same and as a consequence it gives rise to the identical expressions for the temperature in both cases.

  12. Tunnelling of scalar and Dirac particles from squashed charged rotating Kaluza-Klein black holes

    Energy Technology Data Exchange (ETDEWEB)

    Stetsko, M.M. [Ivan Franko National University of Lviv, Department of Theoretical Physics, Lviv (Ukraine)

    2016-02-15

    The thermal radiation of scalar particles and Dirac fermions from squashed charged rotating five-dimensional black holes is considered. To obtain the temperature of the black holes we use the tunnelling method. In the case of scalar particles we make use of the Hamilton-Jacobi equation. To consider tunnelling of fermions the Dirac equation was investigated. The examination shows that the radial parts of the action for scalar particles and fermions in the quasi-classical limit in the vicinity of horizon are almost the same and as a consequence it gives rise to identical expressions for the temperature in the two cases. (orig.)

  13. Tunnelling of scalar and Dirac particles from squashed charged rotating Kaluza-Klein black holes

    Science.gov (United States)

    Stetsko, M. M.

    2016-02-01

    The thermal radiation of scalar particles and Dirac fermions from squashed charged rotating five-dimensional black holes is considered. To obtain the temperature of the black holes we use the tunnelling method. In the case of scalar particles we make use of the Hamilton-Jacobi equation. To consider tunnelling of fermions the Dirac equation was investigated. The examination shows that the radial parts of the action for scalar particles and fermions in the quasi-classical limit in the vicinity of horizon are almost the same and as a consequence it gives rise to identical expressions for the temperature in the two cases.

  14. Scalar field breathers on anti-de Sitter background

    CERN Document Server

    Fodor, Gyula; Grandclément, Philippe

    2013-01-01

    We study spatially localized, time-periodic solutions (breathers) of scalar field theories with various self-interacting potentials on Anti-de Sitter (AdS) spacetimes in $D$ dimensions. A detailed numerical study of spherically symmetric configurations in $D=3$ dimensions is carried out, revealing a rich and complex structure of the phase-space (bifurcations, resonances). Scalar breather solutions form one-parameter families parametrized by their amplitude, $\\varepsilon$, while their frequency, $\\omega=\\omega(\\varepsilon)$, is a function of the amplitude. The scalar breathers on AdS we find have a small amplitude limit, tending to the eigenfunctions of the linear Klein-Gordon operator on AdS. Importantly most of these breathers appear to be generically stable under time evolution.

  15. Inflation with an extra light scalar field after Planck

    CERN Document Server

    Vennin, Vincent; Wands, David

    2015-01-01

    Bayesian inference techniques are used to investigate situations where an additional light scalar field is present during inflation and reheating. This includes (but is not limited to) curvaton-type models. We design a numerical pipeline where $\\simeq 200$ inflaton setups $\\times\\, 10$ reheating scenarios $= 2000$ models are implemented and we present the results for a few prototypical potentials. We find that single-field models are remarkably robust under the introduction of light scalar degrees of freedom. Models that are ruled out at the single-field level are not improved in general, because good values of the spectral index and the tensor-to-scalar ratio can only be obtained for very fine-tuned values of the extra field parameters and/or when large non-Gaussianities are produced. The only exception is quartic large-field inflation, so that the best models after Planck are of two kinds: plateau potentials, regardless of whether an extra field is added or not, and quartic large-field inflation with an ext...

  16. The fluctuation-dissipation dynamics of cosmological scalar fields

    CERN Document Server

    Bartrum, Sam; Rosa, Joao G

    2014-01-01

    We show that dissipative effects have a significant impact on the evolution of cosmological scalar fields, leading to friction, entropy production and field fluctuations. We explicitly compute the dissipation coefficient for different scalar fields within the Standard Model and some of its most widely considered extensions, in different parametric regimes. We describe the generic consequences of fluctuation-dissipation dynamics in the post-inflationary universe and analyze in detail two important effects. Firstly, we show that dissipative friction delays the process of spontaneous symmetry breaking and may even damp the the motion of a Higgs field sufficiently to induce a late period of warm inflation. Along with dissipative entropy production, this may parametrically dilute the abundance of dangerous thermal relics. Secondly, we show that dissipation can generate the observed baryon asymmetry without symmetry restoration, and we develop in detail a model of dissipative leptogenesis. We further show that this...

  17. Dynamical locality of the free scalar field

    CERN Document Server

    Fewster, Christopher J

    2011-01-01

    Dynamical locality is a condition on a locally covariant physical theory, asserting that kinematic and dynamical notions of local physics agree. This condition was introduced in [arXiv:1106.4785], where it was shown to be closely related to the question of what it means for a theory to describe the same physics on different spacetimes. In this paper, we consider in detail the example of the free minimally coupled Klein--Gordon field, both as a classical and quantum theory (using both the Weyl algebra and a smeared field approach). It is shown that the massive theory obeys dynamical locality, both classically and in quantum field theory, in all spacetime dimensions $n\\ge 2$ and allowing for spacetimes with finitely many connected components. In contrast, the massless theory is shown to violate dynamical locality in any spacetime dimension, in both classical and quantum theory, owing to a rigid gauge symmetry. Taking this into account (equivalently, working with the massless current) dynamical locality is resto...

  18. General features of single-scalar field dark energy models

    CERN Document Server

    Perenon, Louis

    2016-01-01

    We present a systematic study of modified gravity (MG) models containing a single scalar field non-minimally coupled to the metric. Despite a large parameter space, exploiting the effective field theory of dark energy (EFT of DE) formulation and imposing simple physical constraints such as stability conditions and (sub-)luminal propagation of perturbations, we arrive at a number of generic predictions about the large scale structures.

  19. Applications of theorems of Jean Leray to the Einstein-scalar field equations

    CERN Document Server

    Choquet-Bruhat, Y; Pollack, D; Choquet-Bruhat, Yvonne; Isenberg, James; Pollack, Daniel

    2006-01-01

    The Einstein-scalar field theory can be used to model gravitational physics with scalar field matter sources. We discuss the initial value formulation of this field theory, and show that the ideas of Leray can be used to show that the Einstein-scalar field system of partial differential equations is well-posed as an evolutionary system. We also show that one can generate solutions of the Einstein-scalar field constraint equations using conformal methods.

  20. Feynman propagator for a free scalar field on a causal set.

    Science.gov (United States)

    Johnston, Steven

    2009-10-30

    The Feynman propagator for a free bosonic scalar field on the discrete spacetime of a causal set is presented. The formalism includes scalar field operators and a vacuum state which define a scalar quantum field theory on a causal set. This work can be viewed as a novel regularization of quantum field theory based on a Lorentz invariant discretization of spacetime.

  1. A Note on Scalar Field Theory in AdS_3/CFT_2

    CERN Document Server

    Minces, Pablo

    2009-01-01

    We consider a scalar field theory in AdS_{d+1}, and introduce a formalism on surfaces at equal values of the radial coordinate. In particular, we define the corresponding conjugate momentum. We compute the Noether currents for isometries in the bulk, and carefully perform the asymptotic limit on the corresponding `conserved' charges. We then introduce Poisson brackets at the border, and show that the asymptotic values of the bulk scalar field and the conjugate momentum transform as conformal fields of scaling dimensions \\Delta_{-} and \\Delta_{+}, respectively, where \\Delta_{\\pm} are the standard parameters giving the asymptotic behavior of the scalar field in AdS. Then we consider the case d=2, where the boundary is described in terms of complex holomorphic and antiholomorphic coordinates. We obtain two copies of the Virasoro algebra, with vanishing central charge. An AdS_3/CFT_2 prescription, giving the commutators of the boundary CFT in terms of the Poisson brackets at the border, arises in a natural way. W...

  2. LHC bounds on lepton number violation mediated by doubly and singly-charged scalars

    International Nuclear Information System (INIS)

    The only possible doubly-charged scalar decays into two Standard Model particles are into pairs of same-sign charged leptons, H±±→l±l±,l=e,μ,τ, or gauge bosons, H±±→W±W±; being necessary the observation of both to assert the violation of lepton number. However, present ATLAS and CMS limits on doubly-charged scalar production are obtained under specific assumptions on its branching fractions into dileptons only. Although they can be extended to include decays into dibosons and lepton number violating processes. Moreover, the production rates also depend on the type of electroweak multiplet H±± belongs to. We classify the possible alternatives and provide the Feynman rules and codes for generating the corresponding signals for pair and associated doubly-charged scalar production, including the leading contribution from the s-channel exchange of electroweak gauge bosons as well as the vector-boson fusion corrections. Then, using the same analysis criteria as the LHC collaborations we estimate the limits on the H±± mass as a function of the electroweak multiplet it belongs to, and obtain the bounds on the lepton number violating processes pp→H±±H∓∓→ℓ±ℓ±W∓W∓ and pp→H±±H∓→ℓ±ℓ±W∓Z, ℓ=e,μ, implied by the ATLAS and CMS doubly-charged scalar searches

  3. Transport coefficients of O(N) scalar field theories close to the critical point

    CERN Document Server

    Nakano, Eiji; Friman, Bengt

    2011-01-01

    We investigate the critical dynamics of O(N)-symmetric scalar field theories to determine the critical exponents of transport coefficients as a second-order phase transition is approached from the symmetric phase. A set of stochastic equations of motion for the slow modes is formulated, and the long wavelength dynamics is examined for an arbitrary number of field components, $N$, in the framework of the dynamical renormalization group within the $\\epsilon$ expansion. We find that for a single component scalar field theory, N=1, the system reduces to the model C of critical dynamics, whereas for $N>1$ the model G is effectively restored owing to dominance of O(N)-symmetric charge fluctuations. In both cases, the shear viscosity remains finite in the critical region. On the other hand, we find that the bulk viscosity diverges as the correlation length squared, for N=1, whereas it remains finite for $N>1$.

  4. STATIC SPHERICALLY SYMMETRIC SOLUTION OF EINSTEIN GRAVITY COUPLED TO ELECTROMAGNETIC AND SCALAR FIELDS

    Institute of Scientific and Technical Information of China (English)

    陈光

    2001-01-01

    The static spherically symmetric solution of Einstein gravity coupled to electromagnetic and scalar fields is obtained under the consideration of the self-gravitational interaction of the electromagnetic and scalar fields, which is singularityfree and stable.

  5. Stability of Scalar Fields in Warped Extra Dimensions

    CERN Document Server

    Aybat, S Mert

    2010-01-01

    This work sets up a general theoretical framework to study stability of models with a warped extra dimension where N scalar fields couple minimally to gravity. Our analysis encompasses Randall-Sundrum models with branes and bulk scalars, and general domain-wall models. We derive the Schrodinger equation governing the spin-0 spectrum of perturbations of such a system. This result is specialized to potentials generated using fake supergravity, and we show that models without branes are free of tachyonic modes. Turning to the existence of zero modes, we prove a theorem relating the number of normalizable zero modes to the parities of the background scalar profiles. Constructions with definite parity and only odd scalar profiles are shown to be free of zero modes and are hence perturbatively stable. We give two explicit examples of domain-wall models with a soft wall, one which admits a zero mode and one which does not. The latter is an example of a model that stabilizes a compact extra dimension using only bulk ...

  6. Scalar field as a Bose-Einstein condensate?

    International Nuclear Information System (INIS)

    We discuss the analogy between a classical scalar field with a self-interacting potential, in a curved spacetime described by a quasi-bounded state, and a trapped Bose-Einstein condensate. In this context, we compare the Klein-Gordon equation with the Gross-Pitaevskii equation. Moreover, the introduction of a curved background spacetime endows, in a natural way, an equivalence to the Gross-Pitaevskii equation with an explicit confinement potential. The curvature also induces a position dependent self-interaction parameter. We exploit this analogy by means of the Thomas-Fermi approximation, commonly used to describe the Bose-Einstein condensate, in order to analyze the quasi bound scalar field distribution surrounding a black hole

  7. Scalar Field Cosmologies Hidden Within the Nonlinear Schrodinger Equation

    CERN Document Server

    Lidsey, James E

    2013-01-01

    The nonlinear, cubic Schrodinger (NLS) equation has numerous physical applications, but in general is very difficult to solve. Nonetheless, under certain circumstances parameters quantifying the width, momentum and energy of the wavefunction evolve under a closed set of ordinary differential equations. It is shown that for the case of the radial, two dimensional NLS equation, such evolution equations may be mapped directly onto the cosmological Friedmann equations for a spatially flat and isotropic universe sourced by a self-interacting scalar field and a barotropic perfect fluid. Consequently, analytical techniques that have been developed to study the dynamics of such cosmological models may be applied to gain insight into aspects of nonlinear quantum mechanics. In this paper, the Hamilton-Jacobi formalism of the Friedmann equations, where the scalar field is viewed as the dynamical variable, is developed within this context. Algorithms for finding exact solutions are presented and the scaling solutions det...

  8. Dynamical dark energy: scalar fields and running vacuum

    CERN Document Server

    Sola, Joan; Perez, Javier de Cruz

    2016-01-01

    Recent analyses in the literature suggest that the concordance $\\Lambda$CDM model with rigid cosmological term, $\\Lambda=$const., may not be the best description of the cosmic acceleration. The class of "running vacuum models", in which $\\Lambda=\\Lambda(H)$ evolves with the Hubble rate, has been shown to fit the string of $SNIa+BAO+H(z)+LSS+CMB$ data significantly better than the $\\Lambda$CDM. Here we provide further evidence on the time-evolving nature of the dark energy (DE) by fitting the same cosmological data in terms of scalar fields. As a representative model we use the original Peebles & Ratra potential, $V\\propto\\Phi^{-\\alpha}$. We find clear signs of dynamical DE at $\\sim 4\\sigma$ c.l., thus reconfirming through a nontrivial scalar field approach the strong hints formerly found with other models and parametrizations.

  9. The scalar field in quantum gravity: a spin foam model

    International Nuclear Information System (INIS)

    Spin foams are nonperturbative models that describe spacetime at the Planck scale. They have been introduced starting from loop quantum gravity, but have consequently been recognized in other approaches. The most prominent of all is the Barrett-Crane model. However, this is a description of pure gravity and various attempts have been made in order to introduce matter in this general setting. The present paper describes the coupling of a massless scalar field to the Riemannian Barrett-Crane model and is, to our best knowledge, the first attempt of this kind. The main result is the computation of the partition function for the coupled model. This exhibits the general structure of a spin foam partition function. It is given by a product of face, edge and vertex amplitudes together with a sum over the irreducible representations of both the gauge group of the scalar field and the gauge group of gravity. (author)

  10. Scalar Field Quantization Without Divergences In All Spacetime Dimensions

    CERN Document Server

    Klauder, John R

    2011-01-01

    Covariant, self-interacting scalar quantum field theories admit solutions for low enough spacetime dimensions, but when additional divergences appear in higher dimensions, the traditional approach leads to results, such as triviality, that are less than satisfactory. Guided by idealized but soluble nonrenormalizable models, a nontraditional proposal for the quantization of covariant scalar field theories is advanced, which achieves a term-by-term, divergence-free, perturbation analysis of interacting models expanded about a suitable pseudofree theory, which differs from a free theory by an O(\\hbar^2) counterterm. These positive features are secured within a functional integral formulation by a local, nonclassical, counterterm that effectively transforms parameter changes in the action from generating mutually singular measures, which are the basis for divergences, to equivalent measures, thereby removing all divergences. The use of an alternative model about which to perturb is already supported by properties...

  11. Scalar field as a Bose-Einstein condensate?

    Energy Technology Data Exchange (ETDEWEB)

    Castellanos, Elías; Escamilla-Rivera, Celia [Mesoamerican Centre for Theoretical Physics (ICTP regional headquarters in Central America, the Caribbean and Mexico), Universidad Autónoma de Chiapas, Carretera Zapata Km. 4, Real del Bosque (Terán), 29040, Tuxtla Gutiérrez, Chiapas (Mexico); Macías, Alfredo [Departamento de Física, Universidad Autónoma Metropolitana-Iztapalapa, A.P. 55-534, Mexico D.F. 09340 (Mexico); Núñez, Darío, E-mail: ecastellanos@mctp.mx, E-mail: cescamilla@mctp.mx, E-mail: amac@xanum.uam.mx, E-mail: nunez@nucleares.unam.mx [Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior C.U., A.P. 70-543, México D.F. 04510 (Mexico)

    2014-11-01

    We discuss the analogy between a classical scalar field with a self-interacting potential, in a curved spacetime described by a quasi-bounded state, and a trapped Bose-Einstein condensate. In this context, we compare the Klein-Gordon equation with the Gross-Pitaevskii equation. Moreover, the introduction of a curved background spacetime endows, in a natural way, an equivalence to the Gross-Pitaevskii equation with an explicit confinement potential. The curvature also induces a position dependent self-interaction parameter. We exploit this analogy by means of the Thomas-Fermi approximation, commonly used to describe the Bose-Einstein condensate, in order to analyze the quasi bound scalar field distribution surrounding a black hole.

  12. Coupled dark energy: a dynamical analysis with complex scalar field

    CERN Document Server

    Landim, Ricardo C G

    2016-01-01

    The dynamical analysis for coupled dark energy with dark matter is presented, where a complex scalar field is taken into account and it is considered in the presence of a barothropic fluid. We consider three dark energy candidates: quintessence, phantom and tachyon. The critical points are found and their stabilities analyzed, leading to the three cosmological eras (radiation, matter and dark energy), for a generic potential. The results presented here enlarge the previous analyses found in the literature.

  13. Higgs particles interacting via a scalar Dark Matter field

    OpenAIRE

    Bhattacharya, Yajnavalkya; Darewych, Jurij W.

    2016-01-01

    We study a system of two Higgs bound state, interacting via a real scalar Dark Matter mediating field, without imposing $Z_2$ symmetry on the DM sector of the postulated Lagrangian. The variational method in the Hamiltonian formalism of QFT is used to derive relativistic wave equations for the two-Higgs system, using a truncated Fock-space trial state. Approximate solutions of the 2-body relativistic coupled integral equations are presented, and conditions for the existence of Higgs bound sta...

  14. Scalar fields in BTZ black hole spacetime and entanglement entropy

    Science.gov (United States)

    Veer Singh, Dharm; Siwach, Sanjay

    2013-12-01

    We study the quantum scalar fields in the background of BTZ black hole spacetime. We calculate the entanglement entropy using the discretized model, which resembles a system of coupled harmonic oscillators. The leading term of the entropy formula is standard Bakenstein-Hawking entropy and sub-leading corresponds to quantum corrections to black hole entropy. We calculate the coefficient of sub-leading logarithmic corrections numerically.

  15. Higgs particles interacting via a scalar Dark Matter field

    Directory of Open Access Journals (Sweden)

    Bhattacharya Yajnavalkya

    2016-01-01

    Full Text Available We study a system of two Higgs particles, interacting via a scalar Dark Matter mediating field. The variational method in the Hamiltonian formalism of QFT is used to derive relativistic wave equations for the two-Higgs system, using a truncated Fock-space trial state. Approximate solutions of the two-body equations are used to examine the existence of Higgs bound states.

  16. Coupled dark energy: a dynamical analysis with complex scalar field

    OpenAIRE

    Landim, Ricardo C. G.

    2016-01-01

    The dynamical analysis for coupled dark energy with dark matter is presented, where a complex scalar field is taken into account and it is considered in the presence of a barothropic fluid. We consider three dark-energy candidates: quintessence, phantom, and tachyon. The critical points are found and their stabilities analyzed, leading to the three cosmological eras (radiation, matter, and dark energy), for a generic potential. The results presented here extend the previous analyses found in ...

  17. Coupled dark energy: a dynamical analysis with complex scalar field

    Energy Technology Data Exchange (ETDEWEB)

    Landim, Ricardo C.G. [Universidade de Sao Paulo, Instituto de Fisica, Caixa Postal 66318, Sao Paulo, SP (Brazil)

    2016-01-15

    The dynamical analysis for coupled dark energy with dark matter is presented, where a complex scalar field is taken into account and it is considered in the presence of a barothropic fluid. We consider three dark-energy candidates: quintessence, phantom, and tachyon. The critical points are found and their stabilities analyzed, leading to the three cosmological eras (radiation, matter, and dark energy), for a generic potential. The results presented here extend the previous analyses found in the literature. (orig.)

  18. Production of Charged Scalars from the Littlest Higgs Model Associated with Top Quark at LHC

    Institute of Scientific and Technical Information of China (English)

    LIU Wei-Na; LIU Yao-Bei; LI Ping; SHEN Jie-Fen; GOU Qing-Quan; CUI Xiao-Min; ZHAO Yan-Ping; REN Xiao-Yan

    2008-01-01

    The littlest Higgs (LH) model is the most economical one among various little Higgs models, which predicts the existence of the charged scalars φ±. In this paper, we study the production of the charged Higgs boson φ- with single top quark via the process gb → tφ- at the CERN Large Hadron Collider (LHC). The numerical results show that the production cross section is smaller than 0.2 pb in most of the parameters space, it is very difficult to observe the signatures of the charged scalars via the process pp → gb + X → tφ- + X at the LHC experiments. However, it can open a window to distinguish the top-pions in the TC2 model or charged Higgs in the MSSM from φ±.

  19. Green's function of a massless scalar field in curved space-time and superluminal phase velocity of the retarded potential

    CERN Document Server

    Dai, De-Chang

    2012-01-01

    We study a retarded potential solution of a massless scalar field in curved space-time. In a special ansatz for a particle at rest whose magnitude of the (scalar) charge is changing with time, we found an exact analytic solution. The solution indicates that the phase velocity of the retarded potential of a non-moving scalar charge is position dependent, and may easily be greater than the speed of light at a given point. In the case of the Schwarzschild space-time, at the horizon, the phase velocity becomes infinitely faster than the coordinate speed of light at that point. Superluminal phase velocity is relatively common phenomenon, with the the phase velocity of the massive Klein-Gordon field as the best known example. We discuss why it is possible to have modes with superluminal phase velocity even for a massless field.

  20. Study of Inflationary Generalized Cosmic Chaplygin Gas for Standard and Tachyon Scalar Fields

    CERN Document Server

    Sharif, M

    2014-01-01

    We consider an inflationary universe model in the context of generalized cosmic Chaplygin gas by taking matter field as standard and tachyon scalar fields. We evaluate the corresponding scalar fields and scalar potentials during intermediate and logamediate inflationary regimes by modifying the first Friedmann equation. In each case, we evaluate the number of e-folds, scalar as well as tensor power spectra, scalar spectral index and important observational parameter, i.e., tensor-scalar ratio in terms of inflatons. The graphical behavior of this parameter shows that the model remains incompatible with WMAP7 and Planck observational data in each case.

  1. Study of inflationary generalized cosmic Chaplygin gas for standard and tachyon scalar fields

    Energy Technology Data Exchange (ETDEWEB)

    Sharif, M.; Saleem, Rabia [University of the Punjab, Department of Mathematics, Lahore (Pakistan)

    2014-07-15

    We consider an inflationary universe model in the context of the generalized cosmic Chaplygin gas by taking the matter field as standard and tachyon scalar fields. We evaluate the corresponding scalar fields and scalar potentials during the intermediate and logamediate inflationary regimes by modifying the first Friedmann equation. In each case, we evaluate the number of e-folds, scalar as well as tensor power spectra, scalar spectral index, and the important observational parameter, the tensor-scalar ratio in terms of inflation. The graphical behavior of this parameter shows that the model remains incompatible with WMAP7 and Planck observational data in each case. (orig.)

  2. On the Energy-Momentum Tensor of the Scalar Field in Scalar--Tensor Theories of Gravity

    OpenAIRE

    Santiago, David I.; Silbergleit, Alexander S.

    1999-01-01

    We study the dynamical description of gravity, the appropriate definition of the scalar field energy-momentum tensor, and the interrelation between them in scalar-tensor theories of gravity. We show that the quantity which one would naively identify as the energy-momentum tensor of the scalar field is not appropriate because it is spoiled by a part of the dynamical description of gravity. A new connection can be defined in terms of which the full dynamical description of gravity is explicit, ...

  3. Quasistationary solutions of scalar fields around accreting black holes

    CERN Document Server

    Sanchis-Gual, Nicolas; Izquierdo, Paula; Font, José A; Montero, Pedro J

    2016-01-01

    Massive scalar fields can form long-lived configurations around black holes. These configurations, dubbed quasi-bound states, have been studied both in the linear and nonlinear regimes. In this paper we show that quasi-bound states can form in a dynamical scenario in which the mass of the black hole grows significantly due to the capture of infalling matter. We solve the Klein-Gordon equation numerically in spherical symmetry, mimicking the evolution of the spacetime through a sequence of analytic Schwarzschild black hole solutions of increasing mass. It is found that the frequency of oscillation of the quasi-bound states decreases as the mass of the black hole increases. In addition, accretion leads to a significative increase of the exponential decay of the scalar field energy due to the presence of terms of order higher than linear in the exponent. We compare the black hole mass growth rates used in our study with estimates from observational surveys and extrapolate our results to values of the scalar fiel...

  4. On the Effects of Coupled Scalar Fields on Structure Formation

    CERN Document Server

    Li, Baojiu

    2010-01-01

    A coupling between a scalar field (representing the dark energy) and dark matter could produce rich phenomena in cosmology. It affects cosmic structure formation mainly through the fifth force, a velocity-dependent force that acts parallel to particle's direction of motion and proportional to its speed, an effective rescaling of the particle masses, and a modified background expansion rate. In many cases these effects entangle and it is difficult to see which is the dominant one. Here we perform N-body simulations to study their qualitative behaviour and relative importance in affecting the key structure formation observables, for a model with exponential scalar field coupling. We find that the fifth force, a prominent example of the scalar-coupling effects, is far less important than the rescaling of particle mass or the modified expansion rate. In particular, the rescaling of particle masses is shown to be the key factor leading to less concentration of particles in halos than in LCDM, a pattern which is al...

  5. Scalar field quantization without divergences in all spacetime dimensions

    Science.gov (United States)

    Klauder, John R.

    2011-07-01

    Covariant, self-interacting scalar quantum field theories admit solutions for low enough spacetime dimensions, but when additional divergences appear in higher dimensions, the traditional approach leads to results, such as triviality, that are less than satisfactory. Guided by idealized but soluble nonrenormalizable models, a nontraditional proposal for the quantization of covariant scalar field theories is advanced, which achieves a term-by-term, divergence-free, perturbation analysis of interacting models expanded about a suitable pseudofree theory, which differs from a free theory by an O(planck2) counterterm. These positive features are realized within a functional integral formulation by a local, nonclassical, counterterm that effectively transforms parameter changes in the action from generating mutually singular measures, which are the basis for divergences, to equivalent measures, thereby removing all divergences. The use of an alternative model about which to perturb is already supported by properties of the classical theory and is allowed by the inherent ambiguity in the quantization process itself. This procedure not only provides acceptable solutions for models for which no acceptable, faithful solution currently exists, e.g. phiv4n, for spacetime dimensions n >= 4, but offers a new, divergence-free solution for less-singular models as well, e.g. phiv4n, for n = 2, 3. Our analysis implies similar properties for multicomponent scalar models, such as those associated with the Higgs model.

  6. Phase space localization of a scalar charged particle

    CERN Document Server

    Semenov, A A

    2002-01-01

    The thesis is devoted to the phase space representation of relativistic quantum mechanics. For a class of observables with matrix-valued Weyl symbols proportional to the identity matrix, the Weyl-Wigner-Moyal formalism is proposed. The evolution equations are found to coincide with their counterparts in relativistic quantum mechanics with non-local Hamiltonian. The difference between the theories is connected with peculiarities of the constraints on the initial conditions. Effective increase in coherence between eigenstates of the Hamiltonian is found. Relativistic coherent states that take into account a non-trivial charge structure of the position and momentum operators and satisfy the charge superselection rule are considered. On this basis, the entangled coherent states are developed.

  7. Orbital angular momentum of scalar field generated by gravitational scatterings

    CERN Document Server

    Nishikawa, Ryusuke; Masuda, Atsuki; Nambu, Yasusada; Ishihara, Hideki

    2016-01-01

    It has been expected that astronomical observations to detect the orbital angular momenta of electromagnetic waves may give us a new insight into astrophysics. Previous works pointed out the possibility that a rotating black hole can produce orbital angular momenta of electromagnetic waves through gravitational scattering, and the spin parameter of the black hole can be measured by observing them. However, the mechanism how the orbital angular momentum of the electromagnetic wave is generated by the gravitational scattering has not been clarified sufficiently. In this paper, in order to understand it from a point of view of gravitational lensing effects, we consider an emitter which radiates a spherical wave of the real massless scalar field and study the deformation of the scalar wave by the gravitational scattering due to a black hole by invoking the geometrical optics approximation. We show that the frame dragging caused by the rotating black hole is not a necessary condition for generating the orbital ang...

  8. Entanglement of self interacting scalar fields in an expanding spacetime

    CERN Document Server

    Alexander, Helder; Mansfield, Paul; da Paz, I G; Sampaio, Marcos

    2016-01-01

    We evaluate self-interaction effects on the quantum correlations of field modes of opposite momenta for scalar $\\lambda \\phi^4$ theory in a two-dimensional asymptotically flat Robertson-Walker spacetime. Such correlations are encoded both in the von-Neumann entropy defined through the reduced density matrix in one of the modes and in the covariance expressed in terms of the expectation value of the number operators for each mode in the evolved state. The entanglement between field modes carries information about the underlying spacetime evolution.

  9. Partition function of massless scalar field in Schwarzschild background

    CERN Document Server

    Sanyal, Abhik Kumar

    2014-01-01

    Using thermal value of zeta function instead of zero temperature, the partition function of quantized fields in arbitrary stationary backgrounds was found to be independent of undetermined regularization constant in even-dimension and the long drawn problem associated with the trace anomaly effect had been removed. Here, we explicitly calculate the expression for the coincidence limit so that the technique may be applied in some specific problems. A particular problem dealt with here is to calculate the partition function of massless scalar field in Schwarzschild background.

  10. Geometrical destabilization of heavy scalar fields during inflation

    CERN Document Server

    Renaux-Petel, Sébastien

    2015-01-01

    We show the existence of a general mechanism by which heavy scalar fields can be destabilized during inflation. It relies on the fact that the effective mass of fluctuations orthogonal to the inflationary direction contains a contribution proportional to the curvature tensor of the field space metric, and that it can render the entropic fluctuations tachyonic. We describe a simple and rather universal setup in which apparently benign higher-order operators trigger this instability. This phenomenon can prematurely end inflation and have important observational consequences, sometimes excluding models that would otherwise perfectly fit the data. More generally, it modifies the interpretation of cosmological constraints in terms of fundamental physics.

  11. Stray magnetic field compensation with a scalar atomic magnetometer

    Science.gov (United States)

    Belfi, J.; Bevilacqua, G.; Biancalana, V.; Cecchi, R.; Dancheva, Y.; Moi, L.

    2010-06-01

    We describe a system for the compensation of time-dependent stray magnetic fields using a dual channel scalar magnetometer based on nonlinear Faraday rotation in synchronously optically pumped Cs vapor. We detail the active control strategy, with an emphasis on the electronic circuitry, based on a simple phase-locked-loop integrated circuit. The performance and limits of the system developed are tested and discussed. The system was applied to significantly improve the detection of free induction decay signals from protons of remotely magnetized water precessing in an ultralow magnetic field.

  12. Stray Magnetic Field Compensation with a Scalar Atomic Magnetometer

    CERN Document Server

    Belfi, Jacopo; Biancalana, Valerio; Cecchi, Roberto; Dancheva, Yordanka; Moi, Luigi

    2010-01-01

    We describe a system for the compensation of time-dependent stray magnetic fields using a dual channel scalar magnetometer based on non-linear Faraday rotation in synchronously optically pumped Cs vapour. We detail the active control strategy, with an emphasis on the electronic circuitry, based on a simple phase-locked-loop integrated circuit. The performance and limits of the system developed are tested and discussed. The system was applied to significantly improve the detection of free induction decay signals from protons of remotely magnetized water precessing in an ultra-low magnetic field.

  13. Mass hierarchies and nondecoupling in multi-scalar-field dynamics

    International Nuclear Information System (INIS)

    In this work, we study the effects of field space curvature on scalar field perturbations around an arbitrary background field trajectory evolving in time. Nontrivial imprints of the 'heavy' directions on the low-energy dynamics arise when the vacuum manifold of the potential does not coincide with the span of geodesics defined by the sigma model metric of the full theory. When the kinetic energy is small compared to the potential energy, the field traverses a curve close to the vacuum manifold of the potential. The curvature of the path followed by the fields can still have a profound influence on the perturbations, as modes parallel to the trajectory mix with those normal to it if the trajectory turns sharply enough. We analyze the dynamical mixing between these nondecoupled degrees of freedom and deduce its nontrivial contribution to the low-energy effective theory for the light modes. We also discuss the consequences of this mixing for various scenarios where multiple scalar fields play a vital role, such as inflation and low-energy compactifications of string theory.

  14. Effects of Interaction Between Gravitation and Nonlinear Electrodynamics On Scalar Field Evolution

    Institute of Scientific and Technical Information of China (English)

    CHEN Ju-Hua; WANG Yong-Jiu

    2011-01-01

    In this paper we investigate the scalar field evolution in the dyadosphere spacetime by using the third-order WKB approximation.We find that the coupling term between the gravitation and the nonlinear electrodynamics makes the scalar field decay more quickly and it also makes the scalar field oscillate more slowly.On the other words, this coupling term takes effect on the scalar field evolution as a damping factor.At the same time these effects become more obvious for the scalar field with higher angle quantum number.

  15. Scalar-field amplitudes in black-hole evaporation

    International Nuclear Information System (INIS)

    We consider the quantum-mechanical decay of a Schwarzschild-like black hole into almost-flat space and weak radiation at a very late time. That is, we are concerned with evaluating quantum amplitudes (not just probabilities) for transitions from initial to final states. In this quantum description, no information is lost because of the black hole. The Lagrangian is taken, in the first instance, to consist of the simplest locally supersymmetric generalization of Einstein gravity and a massless scalar field. The quantum amplitude to go from given initial to final bosonic data in a slightly complexified time-interval T=τexp(-iθ) at infinity may be approximated by the form constxexp(-I), where I is the (complex) Euclidean action of the classical solution filling in between the boundary data. Additionally, in a pure supergravity theory, the amplitude constxexp(-I) is exact. Suppose that Dirichlet boundary data for gravity and the scalar field are posed on an initial spacelike hypersurface extending to spatial infinity, just prior to collapse, and on a corresponding final spacelike surface, sufficiently far to the future of the initial surface to catch all the Hawking radiation. Only in an averaged sense will this radiation have an approximately spherically-symmetric distribution. If the time-interval T had been taken to be exactly real, then the resulting 'hyperbolic Dirichlet boundary-value problem' would, as is well known, not be well posed. Provided instead ('Euclidean strategy') that one takes T complex, as above (0<θ=<π/2), one expects that the field equations become strongly elliptic, and that there exists a unique solution to the classical boundary-value problem. Within this context, by expanding the bosonic part of the action to quadratic order in perturbations about the classical solution, one obtains the quantum amplitude for weak-field final configurations, up to normalization. Such amplitudes are here calculated for weak final scalar fields

  16. How can the Standard model Higgs and also the extensions of the Higgs to Yukawa's scalars be interpreted in the spin-charge-family theory and to what predictions about the Higgs does this theory lead?

    CERN Document Server

    Borstnik, Norma Susana Mankoc

    2013-01-01

    This contribution is to show how does the spin-charge-family theory interpret the assumptions of the standard model, and those extensions of this model, which are trying to see the Yukawa couplings as scalar fields with the family (flavour) charges in the fundamental representations of the group. The purpose of these contribution is i.) to try to understand why the standard model works so well, although its assumptions look quite artificial, and ii.) how do predictions of the spin-charge-family theory about the measurements of the scalar fields differ from predictions of the {\\em standard model}, which has only one scalar field - the Higgs - and also from its more or less direct extensions with Yukawas as the scalar dynamical fields with the family charge in the fundamental or anti-fundamental representation of group.

  17. Sensitivity of atom interferometry to ultralight scalar field dark matter

    CERN Document Server

    Geraci, Andrew A

    2016-01-01

    We discuss the use of atom interferometry as a tool to search for Dark Matter (DM) composed of ultra-light scalar fields. Previous work on ultra-light DM detection using accelerometers has considered the possibility of equivalence principle violating effects whereby gradients in the dark matter field can directly produce relative accelerations between media of differing composition. In atom interferometers, we find that time-varying phase signals from oscillatory, or dilaton-like, DM can also arise due to changes in the atom rest mass that can occur between light-pulses throughout the interferometer sequence as well as changes in the earth's gravitational field. We estimate that several orders of magnitude of unexplored phase space for light DM fields can be probed with our proposed method.

  18. Scalar field collapse in a conformally flat spacetime

    CERN Document Server

    Chakrabarti, Soumya

    2016-01-01

    The collapse scenario of a scalar field along with a perfect fluid distribution is investigated for a conformally flat spacetime. The theorem for the integrability of an anharmonic oscillator has been utilized. For a pure power law potential of the form ${\\phi}^{n+1}$, it is found that a central singularity is formed which is covered by an apparent horizon for $n>0$ and $n<-3$. Some numerical results have also been presented for a combination of two different powers of $\\phi$ in the potential.

  19. Slowly rotating scalar field wormholes: The second order approximation

    International Nuclear Information System (INIS)

    We discuss rotating wormholes in general relativity with a scalar field with negative kinetic energy. To solve the problem, we use the assumption about slow rotation. The role of a small dimensionless parameter plays the ratio of the linear velocity of rotation of the wormhole's throat and the velocity of light. We construct the rotating wormhole solution in the second-order approximation with respect to the small parameter. The analysis shows that the asymptotical mass of the rotating wormhole is greater than that of the nonrotating one, and the null energy condition violation in the rotating wormhole spacetime is weaker than that in the nonrotating one.

  20. Revisiting the quantum scalar field in spherically symmetric quantum gravity

    CERN Document Server

    Borja, Enrique F; Strobel, Eckhard

    2012-01-01

    We extend previous results in spherically symmetric gravitational systems coupled with a massless scalar field within the loop quantum gravity framework. As starting point, we take the Schwarzschild spacetime. The results presented here rely on the uniform discretization method. We are able to minimize the associated discrete master constraint using a variational method. The trial state for the vacuum consists of a direct product of a Fock vacuum for the matter part and a Gaussian centered around the classical Schwarzschild solution. This paper follows the line of research presented by Gambini, Pullin and Rastgoo and a comparison between their result and the one given in this work is made.

  1. Complex solutions for the scalar field model of the Universe

    Science.gov (United States)

    Lyons, Glenn W.

    1992-08-01

    The Hartle-Hawking proposal is implemented for Hawking's scalar field model of the Universe. For this model the complex saddle-point geometries required by the semiclassical approximation to the path integral cannot simply be deformed into real Euclidean and real Lorentzian sections. Approximate saddle points are constructed which are fully complex and have contours of real Lorentzian evolution. The semiclassical wave function is found to give rise to classical spacetimes at late times and extra terms in the Hamilton-Jacobi equation do not contribute significantly to the potential.

  2. Five-Dimensional Warped Geometry with a Bulk Scalar Field

    CERN Document Server

    Ito, M

    2001-01-01

    We explore the diversity of warped metric function in five-dimensional gravity including a scalar field and a 3-brane. We point out that the form of the function is determined by a parameter introduced here. For a particular value of the parameter, the warped metric function is smooth without having a singularity, and we show that the bulk cosmological constant have a upper bound and must be positive and that the lower bound of five-dimensional fundamental scale is controlled by both the brane tension and four-dimensional effective Planck scale. The general warp factor obtained here may relate to models inspired by SUGRA or M-theory.

  3. Observable Effects of Scalar Fields and Varying Constants

    CERN Document Server

    Barrow, J D; Barrow, John D.; Shaw, Douglas J.

    2006-01-01

    We show by using the method of matched asymptotic expansions that a sufficient condition can be derived which determines when a local experiment will detect the cosmological variation of a scalar field which is driving the spacetime variation of a supposed constant of Nature. We extend our earlier analyses of this problem by including the possibility that the local region is undergoing collapse inside a virialised structure, like a galaxy or galaxy cluster. We show by direct calculation that the sufficient condition is met to high precision in our own local region and we can therefore legitimately use local observations to place constraints upon the variation of "constants" of Nature on cosmological scales.

  4. Stable cosmological models driven by a free quantum scalar field

    Energy Technology Data Exchange (ETDEWEB)

    Dappiaggi, C.; Pinamonti, N. [Hamburg Univ. (Germany). 2. Inst. fuer Theoretische Physik]|[Citta Univ., Roma (Italy). Istituto Nazionale di Alta Matematica ' ' F. Severi' ' - GNFM; Fredenhagen, K. [Hamburg Univ. (Germany). 2. Inst. fuer Theoretische Physik

    2008-01-15

    In the mathematically rigorous analysis of semiclassical Einstein's equations, the renormalisation of the stress-energy tensor plays a crucial role. We address such a topic in the case of a scalar field with both arbitrary mass and coupling with gravity in the hypothesis that the underlying algebraic quantum state is of Hadamard type. Particularly, if we focus on highly symmetric solutions of the semiclassical Einstein's equations, the envisaged method displays a de Sitter type behaviour even without an a priori introduced cosmological constant. As a further novel result we shall show that these solutions turn out to be stable. (orig.)

  5. Higgs particles interacting via a scalar Dark Matter field

    CERN Document Server

    Bhattacharya, Yajnavalkya

    2016-01-01

    We study a system of two Higgs bound state, interacting via a real scalar Dark Matter mediating field, without imposing $Z_2$ symmetry on the DM sector of the postulated Lagrangian. The variational method in the Hamiltonian formalism of QFT is used to derive relativistic wave equations for the two-Higgs system, using a truncated Fock-space trial state. Approximate solutions of the 2-body relativistic coupled integral equations are presented, and conditions for the existence of Higgs bound states is examined in a broad parameter space of DM mass and coupling constants.

  6. Disformal scalar fields and the dark sector of the universe

    Energy Technology Data Exchange (ETDEWEB)

    Zumalacárregui, M.; Ruiz-Lapuente, P. [Institut de Ciencies del Cosmos, Universitat de Barcelona Marti i Franques 1, E-08028 Barcelona (Spain); Koivisto, T.S. [Institute for Theoretical Physics and the Spinoza Institute, Utrecht University, Leuvenlaan 4, Postbus 80.195, 3508 TD Utrecht (Netherlands); Mota, D.F., E-mail: miguelzuma@am.ub.es, E-mail: t.s.koivisto@uu.nl, E-mail: d.f.mota@astro.uio.no, E-mail: pilar@am.ub.es [Institute of Theoretical Astrophysics, University of Oslo, 0315 Oslo (Norway)

    2010-05-01

    Disformal transformations have proven to be very useful to devise models of the dark sector. In the present paper we apply such transformation to a single scalar field theory as a way to drive the field into a slow roll phase. The canonical scalar field Lagrangian, when coupled to a disformal metric, turns out to have relations to bimetric dark matter theories and to describe many specific dark energy models at various limits, thus providing a surprisingly simple parametrisation of a wide variety of models including tachyon, Chaplygin gas, K-essence and dilatonic ghost condensate. We investigate the evolution of the background and linear perturbations in disformal quintessence in order to perform a full comparison of the predictions with the cosmological data. The dynamics of the expansion, in particular the mechanism of the transition to accelerating phase, is described in detail. We then study the effects of disformal quintessence on cosmic microwave background (CMB) anisotropies and large scale structures (LSS). A likelihood analysis using the latest data on wide-ranging SNIa, CMB and LSS observations is performed allowing variations in six cosmological parameters and the two parameters specifying the model. We find that while a large region of parameter space remains compatible with observations, models featuring either too much early dark energy or too slow transition to acceleration are ruled out.

  7. Probing the Origin of Neutrino Masses and Mixings via Doubly Charged Scalars: Complementarity of the Intensity and the Energy Frontiers

    CERN Document Server

    Geib, Tanja; Merle, Alexander; No, Jose Miguel; Panizzi, Luca

    2015-01-01

    We discuss how the intensity and the energy frontiers provide complementary constraints within a minimal model of neutrino mass involving just one new field beyond the Standard Model at accessible energy, namely a doubly charged scalar $S^{++}$ and its antiparticle $S^{--}$. In particular we focus on the complementarity between high-energy LHC searches and low-energy probes such as lepton flavor violation. Our setting is a prime example of how high- and low-energy physics can cross-fertilize each other.

  8. Probing the origin of neutrino masses and mixings via doubly charged scalars: Complementarity of the intensity and the energy frontiers

    Science.gov (United States)

    Geib, Tanja; King, Stephen F.; Merle, Alexander; No, Jose Miguel; Panizzi, Luca

    2016-04-01

    We discuss how the intensity and the energy frontiers provide complementary constraints within a minimal model of neutrino mass involving just one new field beyond the Standard Model at accessible energy, namely a doubly charged scalar S++ and its antiparticle S-- . In particular, we focus on the complementarity between high-energy LHC searches and low-energy probes such as lepton flavor violation. Our setting is a prime example of how high- and low-energy physics can cross-fertilize each other.

  9. Stable, Renormalizable, Scalar Tachyonic Quantum Field Theory with Chronology Protection

    CERN Document Server

    Radzikowski, Marek J

    2008-01-01

    We use microlocal arguments to suggest that Lorentz symmetry breaking must occur in a reasonably behaved tachyonic quantum field theory that permits renormalizability. In view of this, we present a scalar tachyonic quantum field model with manifestly broken Lorentz symmetry and without exponentially growing/decaying modes. A notion of causality, in which anti-telephones are excluded, and which is viewed as a form of chronology protection, is obeyed. The field theory is constructed in a preferred tachyon frame in terms of commuting creation/annihilation operators. We calculate some sample (renormalized) operators in this preferred frame, argue that the Hadamard condition is satisfied, and discuss the PCT and spin-statistics theorems for this model.

  10. Conformally coupled scalar black holes admit a flat horizon due to axionic charge

    CERN Document Server

    Bardoux, Yannis; Charmousis, Christos

    2012-01-01

    Static, charged black holes in the presence of a negative cosmological constant and with a planar horizon are found in four dimensions. The solutions have scalar secondary hair. We claim that these constitute the planar version of the Martinez-Troncoso-Zanelli black holes, only known up to now for a curved event horizon in four dimensions. Their planar version is rendered possible due to the presence of two, equal and homogeneously distributed, axionic charges dressing the flat horizon. The solutions are presented in the conformal and minimal frame and their basic properties and thermodynamics analysed. Entertaining recent applications to holographic superconductors, we expose two branches of solutions: the undressed axionic Reissner-Nordstrom-AdS black hole, and the novel black hole carrying secondary hair. We show that there is a critical temperature at which the (bald) axionic Reissner-Nordstrom-AdS black hole undergoes a second order phase transition to the hairy black hole spontaneously acquiring scalar ...

  11. Families of stable and metastable solitons in coupled system of scalar fields

    CERN Document Server

    Riazi, Nematollah

    2011-01-01

    In this paper, we obtain stable and metastable soliton solutions of a coupled system of two real scalar fields with five five discrete points of vacua. These solutions have definite topological charges and rest energies and show classical dynamical stability. From a quantum point of view, however, the V-type solutions are expected to be unstable and decay to D-type solutions. The induced decay of a V-type soliton into two D-type ones is calculated numerically, and shown to be chiral, in the sense that the decay products do not respect left-right symmetry.

  12. Pair production of charged scalars and lepton flavor violating signals in the littlest Higgs model at $e^{+}e^{-}$ colliders

    CERN Document Server

    Cagil, Ayse

    2010-01-01

    In this work pair productions of charged and doubly charged scalars in the framework of littlest Higgs model at $e^+e^-$ colliders are studied. In the allowed parameter space of the littlest Higgs model, the production rates of the scalar pairs are calculated. It is obtained that pair productions of charged and doubly charged scalars are reachable at $e^+ e^-$ colliders with energy $\\sqrt{S}\\geq 1.7TeV$. Using the lepton flavor violating decays of charged scalars calculated in literature, final state analysis is done for pair production processes. This analysis show that depending on the model parameters, lepton number and lepton flavor violations can be observed free from any backgrounds.

  13. Time evolutions of scalar field perturbations in D-dimensional Reissner–Nordström Anti-de Sitter black holes

    Directory of Open Access Journals (Sweden)

    Ran Li

    2016-07-01

    Full Text Available Reissner–Nordström Anti-de Sitter (RNAdS black holes are unstable against the charged scalar field perturbations due to the well-known superradiance phenomenon. We present the time domain analysis of charged scalar field perturbations in the RNAdS black hole background in general dimensions. We show that the instabilities of charged scalar field can be explicitly illustrated from the time profiles of evolving scalar field. By using the Prony method to fit the time evolution data, we confirm the mode that dominates the long time behavior of scalar field is in accordance with the quasinormal mode from the frequency domain analysis. The superradiance origin of the instability can also be demonstrated by comparing the real part of the dominant mode with the superradiant condition of charged scalar field. It is shown that all the unstable modes are superradiant, which is consistent with the analytical result in the frequency domain analysis. Furthermore, we also confirm there exists the rapid exponential growing modes in the RNAdS case, which makes the RNAdS black hole a good test ground to investigate the nonlinear evolution of superradiant instability.

  14. Scalar Field Dark Matter in Clusters of Galaxies

    CERN Document Server

    Bernal, Tula; Matos, Tonatiuh

    2016-01-01

    One alternative to the CDM paradigm is the Scalar Field Dark Matter (SFDM) model, which assumes dark matter is a spin-0 ultra-light scalar field with a typical mass $m\\sim10^{-22}\\mathrm{eV}/c^2$ and positive self-interactions. Due to the ultra-light boson mass, the SFDM could form Bose-Einstein condensates in the very early universe, which are interpreted as the dark matter haloes. Although cosmologically the model behaves as CDM, they differ at small scales: SFDM naturally predicts fewer satellite haloes, cores in dwarf galaxies and the formation of massive galaxies at high redshifts. The ground state (or BEC) solution at zero temperature suffices to describe low-mass galaxies but fails for larger systems. A possible solution is adding finite-temperature corrections to the SF potential which allows combinations of excited states. In this work we test the finite-temperature multistate SFDM solution at galaxy cluster scales and compare our results with the NFW and BEC profiles. We achieve this by fitting the ...

  15. Strong deflection lensing by charged black holes in scalar-tensor gravity

    Energy Technology Data Exchange (ETDEWEB)

    Eiroa, Ernesto F.; Sendra, Carlos M. [Instituto de Astronomia y Fisica del Espacio (IAFE, CONICET-UBA), Buenos Aires (Argentina); Universidad de Buenos Aires, Departamento de Fisica, Facultad de Ciencias Exactas y Naturales, Buenos Aires (Argentina)

    2014-11-15

    We examine a class of charged black holes in scalar-tensor gravity as gravitational lenses. We find the deflection angle in the strong deflection limit, from which we obtain the positions and the magnifications of the relativistic images. We compare our results with those corresponding to the Reissner-Norstroem spacetime and we analyze the observational aspects in the case of the Galactic supermassive black hole. (orig.)

  16. Boson Stars in a Theory of Complex Scalar Fields coupled to $U(1)$ Gauge Field and Gravity

    CERN Document Server

    Kumar, Sanjeev; Kulshreshtha, Daya Shankar

    2016-01-01

    We study boson shells and boson stars in a theory of complex scalar field coupled to the $U(1)$ gauge field $A_{\\mu}$ and Einstein gravity with the potential: $V(|\\Phi|) := \\frac{1}{2} m^{2} \\left(|\\Phi|+ a \\right)^2$. This could be considered either as a theory of massive complex scalar field coupled to electromagnetic field and gravity in a conical potential or as a theory in the presence of a potential which is an overlap of a parabolic and a conical potential. Our theory has a positive cosmological constant $(\\Lambda := 4 \\pi G m^2 a^2)$. Boson stars are found to come in two types, having either ball-like or shell-like charge density. We have studied the properties of these solutions and have also determined their domains of existence for some specific values of the parameters of the theory. Similar solutions have also been obtained by Kleihaus, Kunz, Laemmerzahl and List, in a V-shaped scalar potential.

  17. Quark scalar, axial and tensor charges in the Schwinger-Dyson formalism

    International Nuclear Information System (INIS)

    The quark scalar, axial and tensor charges of nucleon are calculated in the Schwinger-Dyson formalism. We first calculate these charges in the rainbow-ladder truncation using the IR cut quark-gluon vertex, and show that the result is in agreement with the known data. We then perform the same calculation with the phenomenological IR singular quark-gluon vertex. In this case, the Schwinger-Dyson equation does not converge. We show that this result suggests the requirement of additional corrections to the rainbow-ladder truncation, due to the interaction between quark and gluons in the deep IR region

  18. Quark scalar, axial and tensor charges in the Schwinger-Dyson formalism

    Energy Technology Data Exchange (ETDEWEB)

    Yamanaka, Nodoka [2-1 Hirosawa, Wako, 351-0198 Saitama (Japan)

    2016-01-22

    The quark scalar, axial and tensor charges of nucleon are calculated in the Schwinger-Dyson formalism. We first calculate these charges in the rainbow-ladder truncation using the IR cut quark-gluon vertex, and show that the result is in agreement with the known data. We then perform the same calculation with the phenomenological IR singular quark-gluon vertex. In this case, the Schwinger-Dyson equation does not converge. We show that this result suggests the requirement of additional corrections to the rainbow-ladder truncation, due to the interaction between quark and gluons in the deep IR region.

  19. A search for charged scalar particles pair produced in e+e- annihilation

    International Nuclear Information System (INIS)

    We have searched for unstable charged scalar particles (S+-) such as techni-pions or charged Higgs particles pair produced in high energy e+e- annihilation. No evidence for such particles was observed in both decay modes e+e- → S+S- → (tauν)(hadrons) and → (tauν)(tauν). Upper limits of 4 to 11% are obtained for the branching ratio S+- → (tauν) in the S+- mass range between 4 to 12 GeV. (orig.)

  20. Quantization of massive scalar fields over static black string backgrounds

    CERN Document Server

    Piedra, Owen Pavel Fernandez

    2007-01-01

    The renormalized mean value of the corresponding components of the Energy-Momentum tensor for massive scalar fields coupled to an arbitrary gravitational field configuration having cylindrical symmetry are analytically evaluated using the Schwinger-DeWitt approximation, up to second order in the inverse mass value. The general results are employed to explicitly derive compact analytical expressions for the Energy-Momentum tensor in the particular background of the Black-String spacetime. In the case of the Black String considered in this work, we proof that a violation of the weak energy condition occur at the horizon of the space-time for values of the coupling constant, that include as particular cases the most interesting of minimal and conformal coupling.

  1. Locally smeared operator product expansions in scalar field theory

    CERN Document Server

    Monahan, Christopher

    2015-01-01

    We propose a new "locally smeared operator product expansion" (sOPE) to decompose non-local operators in terms of a basis of smeared operators. The sOPE formally connects nonperturbative matrix elements determined numerically using lattice field theory to matrix elements of non-local operators in the continuum. These nonperturbative matrix elements do not suffer from power-divergent mixing on the lattice, which significantly complicates calculations of quantities such as the moments of parton distribution functions, provided the smearing scale is kept fixed in the continuum limit. The presence of this smearing scale complicates the connection to the Wilson coefficients of the standard operator product expansion and requires the construction of a suitable formalism. We demonstrate the feasibility of our approach with examples in real scalar field theory.

  2. Coherent Scalar Field Oscillations and the Epoch of Deceleration

    CERN Document Server

    Jackson, J C

    2001-01-01

    The discovery of supernova SN 1997ff at z~1.7 has confirmed the expected switch from cosmological acceleration to deceleration, as predicted by the concordance Lambda/CDM model. However, its position in the SN Ia Hubble diagram suggestes that the switch is too pronounced, which here is taken to mean that a cosmological constant is not an adequate description of the state of the vacuum. An 'oscillessence' model is invoked, with a scalar field phi governed by a simple quadratic potential, which gives a better fit to the new data point. The field is undergoing coherent oscillations, and a key feature of the proposal is that we are towards the end of the second period of acceleration; a Lambda/phi mix replaces Lambda/CDM, with Omega_Lambda~0.4 and Omega_phi~0.6.

  3. Self Tuning Scalar Fields in Spherically Symmetric Spacetimes

    CERN Document Server

    Appleby, Stephen

    2015-01-01

    We search for self tuning solutions to the Einstein-scalar field equations for the simplest class of `Fab-Four' models with constant potentials. We first review the conditions under which self tuning occurs in a cosmological spacetime, and by introducing a small modification to the original theory - introducing the second and third Galileon terms - show how one can obtain de Sitter states where the expansion rate is independent of the vacuum energy. We then consider whether the same self tuning mechanism can persist in a spherically symmetric inhomogeneous spacetime. We show that there are no asymptotically flat solutions to the field equations in which the vacuum energy is screened, other than the trivial one (Minkowski space). We then consider the possibility of constructing Schwarzschild de Sitter spacetimes for the modified Fab Four plus Galileon theory. We argue that the only model that can successfully screen the vacuum energy in both an FLRW and Schwarzschild de Sitter spacetime is one containing `John...

  4. Massless Interacting Scalar Fields in de Sitter space

    CERN Document Server

    Nacir, Diana López; Trombetta, Leonardo G

    2016-01-01

    We present a method to compute the two-point functions for an $O(N)$ scalar field model in de Sitter spacetime, avoiding the well known infrared problems for massless fields. The method is based on an exact treatment of the Euclidean zero modes and a perturbative one of the nonzero modes, and involves a partial resummation of the leading secular terms. This resummation, crucial to obtain a decay of the correlation functions, is implemented along with a double expansion in an effective coupling constant $\\sqrt\\lambda$ and in $1/N$. The results reduce to those known in the leading infrared approximation and coincide with the ones obtained directly in Lorentzian de Sitter spacetime in the large $N$ limit. The new method allows for a systematic calculation of higher order corrections both in $\\sqrt\\lambda$ and in $1/N$.

  5. Complete Hamiltonian analysis of cosmological perturbations at all orders II: Non-canonical scalar field

    CERN Document Server

    Nandi, Debottam

    2016-01-01

    In this work, we present a consistent Hamiltonian analysis of cosmological perturbations for generalized non-canonical scalar fields. In order to do so, we introduce a new phase-space variable that is uniquely defined for different non-canonical scalar fields. We also show that this is the simplest and efficient way of expressing the Hamiltonian. We extend the Hamiltonian approach of [arXiv:1512.02539] to non-canonical scalar field and obtain a new definition of speed of sound in phase-space. In order to invert generalized phase-space Hamilton's equations to Euler-Lagrange equations of motion, we prescribe a general inversion formulae and show that our approach for non-canonical scalar field is consistent. We also obtain the third and fourth order interaction Hamiltonian for generalized non-canonical scalar fields and briefly discuss the extension of our method to generalized Galilean scalar fields.

  6. Cosmological Model with Nonminimal Derivative Coupling of Scalar Fields in Five Dimensions

    CERN Document Server

    Suroso, Agus

    2014-01-01

    We study a nonminimal derivative coupling (NMDC) of scalar field, where the scalar field is coupled to curvature tensor in the five dimensional universal extra dimension model. We apply the Einstein equation and find its solution. First, we consider a special case of pure free scalar field without NMDC and we find that for static extradimension, the solution is equivalent to the standard cosmology with stiff matter. For a general case of pure free scalar field with NMDC, we find that the de Sitter solution is the solution of our model. For this solution, the scalar field evolves linearly in time. In the limit of small Hubble parameter, the general case give us the same solution as in the pure free scalar field. Finally, we perform a dynamical analysis to determine the stability of our model. We find that the extradimension, if it exist, can not be static and always shrinks with the expansion of four dimensional spacetime.

  7. Backreaction to wormhole by classical scalar field: Will classical scalar field destroy wormhole?

    OpenAIRE

    Kim, Sung-Won

    1999-01-01

    There are two effects of extra matter fields on the Lorentzian traversable wormhole. The ``primary effect'' says that the extra matter can afford to be a part of source or whole source of the wormhole when the wormhole is being formed. Thus the matter does not affect the stability of wormhole and the wormhole is still safe. If the extra matter is extotic, it can be the whole part of the source of the wormhole. The ``auxiliary effect'' is that the extra matter plays the role of the additional ...

  8. Comments on Unified dark energy and dark matter from a scalar field different from quintessence

    OpenAIRE

    Chimento, Luis P.; Forte, Mónica

    2010-01-01

    In a recent paper by C. Gao, M. Kunz, A. Liddle and D. Parkinson [arXiv:0912.0949], the unification of dark matter and dark energy was explored within a theory containing a scalar field of non-Lagrangian type. This scalar field, different from the classic quintessence, can be obtained from the scalar field representation of an interacting two-fluid mixture described in the paper by L.P. Chimento and M. Forte [arXiv:0706.4142

  9. Neutron Star Structure in the Presence of Conformally Coupled Scalar Fields

    Science.gov (United States)

    Sultana, Joseph; Bose, Benjamin; Kazanas, Demosthenes

    2014-01-01

    Neutron star models are studied in the context of scalar-tensor theories of gravity in the presence of a conformally coupled scalar field, using two different numerical equations of state (EoS) representing different degrees of stiffness. In both cases we obtain a complete solution by matching the interior numerical solution of the coupled Einstein-scalar field hydrostatic equations, with an exact metric on the surface of the star. These are then used to find the effect of the scalar field and its coupling to geometry, on the neutron star structure, particularly the maximum neutron star mass and radius. We show that in the presence of a conformally coupled scalar field, neutron stars are less dense and have smaller masses and radii than their counterparts in the minimally coupled case, and the effect increases with the magnitude of the scalar field at the center of the star.

  10. The Qualitative and Numerical Analysis of the Cosmological Model Based on Phantom Scalar Field with Self

    CERN Document Server

    Ignat'ev, Yu G

    2016-01-01

    In this paper we investigate the asymptotic behavior of the cosmological model based on phantom scalar field on the ground of qualitative analysis of the system of the cosmological model's differential equations and show that as opposed to models with classical scalar field, such models have stable asymptotic solutions with constant value of the potential both in infinite past and infinite future. We also develop numerical models of the cosmological evolution models with phantom scalar field in this paper. {\\bf keywords}: cosmological model, phantom scalar field, quality analysis, asymptotic behavior, numerical simulation, numerical gravitation.\\\\ {\\bf PACS}: 04.20.Cv, 98.80.Cq, 96.50.S 52.27.Ny

  11. Scalar Field Model of Dark Energy In the Double Complex Symmetric Gravitational Theory

    Institute of Scientific and Technical Information of China (English)

    SHAO Ying; GUI Yuan-Xing; WANG Wei

    2006-01-01

    The scalar field model of dark energy is established in the double complex symmetric gravitational theory. The universe we live in is taken as the real part of double complex space M4C(J). The two cases of scalar field (ordinary and phantom scalar field) are discussed in a unified way. Not only can the double Friedmann equations be obtained, but also the equation of state for dark energy, potential V(φ) and scalar field φ can be expressed. Hence, a new method is proposed to study dark energy and the evolution of the universe.

  12. Gravitomagnetic effects in quadratic gravity with a scalar field

    CERN Document Server

    Finch, Andrew

    2016-01-01

    The two gravitomagnetic effects which influence bodies orbiting around a gravitational source are the geodetic effect and the Lense-Thirring effect. The former describes the precession angle of the axis of a spinning gyroscope while in orbit around a nonrotating gravitational source whereas the latter provides a correction for this angle in the case of a spinning source. In this paper we derive the relevant equations in quadratic gravity and relate them to their equivalents in general relativity. Starting with an investigation into Kepler's third law in quadratic gravity with a scalar field, the effects of an axisymmetric and rotating gravitational source on an orbiting body in a circular, equatorial orbit are introduced.

  13. The Real Scalar Field in Schwarzschild-de Sitter Spacetime

    CERN Document Server

    Tian, J; Guo, G; Lv, Y; Zhang, S; Wang, W; Tian, Jianxiang; Gui, Yuanxing; Guo, Guanghai; Lv, Yan; Zhang, Suhong; Wang, Wei

    2003-01-01

    In this paper, the real scalar field equation in Schwarzschild-de Sitter spacetime is solved numerically with high precision. A method called polynomial approximation is introduced to derive the relation between the tortoise coordinate x and the radius r. This method is different from the tangent approximation [1] and leads to more accurate result. The Nariai black hole is then discussed in details. We find that the wave function is harmonic only near the horizons as I. Brevik and B. Simonsen [1] found. Howerver the wave function is not harmonic in the region of the potential peak, with amplitude increasing instead. Furthermore, we also find that, when cosmological constant decreases, the potential peak increases, and the maximum wave amplitude increases.

  14. Qualitative analysis and characterization of two cosmologies including scalar fields

    CERN Document Server

    Leon, Genly

    2014-01-01

    The problem of dark energy can be roughly stated as the proposition and validation of a cosmological model that can explain the phenomenon of the accelerated expansion of the Universe. This problem is an open discussion topic in modern physics. One of the most common approaches is that of the "Dark Energy" (DE), a matter component still unknown, with repulsive character (to explain the accelerated expansion), which fills about 2/3 of the total content of the Universe. In this thesis are investigated two cosmological models, a non-minimally coupled quintessence field, based on a Scalar-Tensor Theory of gravity, formulated in the Einstein's frame, and a quintom dark energy model, based on General Relativity. A normalization and parametrization procedure is introduced for each model, in order to investigate the flow properties of an associated autonomous system of ordinary differential equations. In our study are combined topological, analytical and numerical techniques. We are mainly interested in the past dyna...

  15. Revisiting the quantum scalar field in spherically symmetric quantum gravity

    Science.gov (United States)

    Borja, Enrique F.; Garay, Iñaki; Strobel, Eckhard

    2012-07-01

    We extend previous results in spherically symmetric gravitational systems coupled with a massless scalar field within the loop quantum gravity framework. As a starting point, we take the Schwarzschild spacetime. The results presented here rely on the uniform discretization method. We are able to minimize the associated discrete master constraint using a variational method. The trial state for the vacuum consists of a direct product of a Fock vacuum for the matter part and a Gaussian centered around the classical Schwarzschild solution. This paper follows the line of research presented by Gambini et al (2009 Class. Quantum Grav. 26 215011 (arXiv:0906.1774v1)) and a comparison between their result and the one given in this work is made.

  16. Polymer-Fourier quantization of the scalar field revisited

    CERN Document Server

    Garcia-Chung, Angel

    2016-01-01

    The Polymer Quantization of the Fourier modes of the real scalar field is studied within algebraic scheme. We replace the positive linear functional of the standard Poincar\\'e invariant quantization by a singular one. This singular positive linear functional is constructed as mimicking the singular limit of the complex structure of the Poincar\\'e invariant Fock quantization. The resulting symmetry group of such Polymer Quantization is the subgroup $\\mbox{SDiff}(\\mathbb{R}^4)$ which is a subgroup of $\\mbox{Diff}(\\mathbb{R}^4)$ formed by spatial volume preserving diffeomorphisms. In consequence, this yields an entirely different irreducible representation of the Canonical Commutation Relations, non-unitary equivalent to the standard Fock representation. We also compared the Poincar\\'e invariant Fock vacuum with the Polymer Fourier vacuum.

  17. Nonequlibrium dynamics of scalar fields in a thermal bath

    Energy Technology Data Exchange (ETDEWEB)

    Anisimov, A.; Buchmueller, W.; Drewes, M.; Mendizabal, S.

    2008-12-15

    We study the approach to equilibrium for a scalar field which is coupled to a large thermal bath. Our analysis of the initial value problem is based on Kadanoff-Baym equations which are shown to be equivalent to a stochastic Langevin equation. The interaction with the thermal bath generates a temperature-dependent spectral density, either through decay and inverse decay processes or via Landau damping. In equilibrium, energy density and pressure are determined by the Bose-Einstein distribution function evaluated at a complex quasi-particle pole. The time evolution of the statistical propagator is compared with solutions of the Boltzmann equations for particles as well as quasi-particles. The dependence on initial conditions and the range of validity of the Boltzmann approximation are determined. (orig.)

  18. Detailed ultraviolet asymptotics for AdS scalar field perturbations

    CERN Document Server

    Evnin, Oleg

    2016-01-01

    We present a range of methods suitable for accurate evaluation of the leading asymptotics for integrals of products of Jacobi polynomials in limits when the degrees of some or all polynomials inside the integral become large. The structures in question have recently emerged in the context of effective descriptions of small amplitude perturbations in anti-de Sitter (AdS) spacetime. The limit of high degree polynomials corresponds in this situation to effective interactions involving extreme short-wavelength modes, whose dynamics is crucial for the turbulent instabilities that determine the ultimate fate of small AdS perturbations. We explicitly apply the relevant asymptotic techniques to the case of a self-interacting probe scalar field in AdS and extract a detailed form of the leading large degree behavior, including closed form analytic expressions for the numerical coefficients appearing in the asymptotics.

  19. Approximation of the potential in scalar field dark energy models

    CERN Document Server

    Battye, Richard A

    2016-01-01

    We study the nature of potentials in scalar field based models for dark energy - both with canonical and non-canonical kinetic terms. We calculate numerically, and using an analytic approximation around $a\\approx 1$, potentials for models with constant equation-of-state parameter, $w_{\\phi}$. We find that for a wide range of models with canonical and non-canonical kinetic terms there is a simple approximation for the potential that holds when the scale factor is in the range $0.6\\lesssim a\\lesssim 1.4$. We discuss how this form of the potential can also be used to represent models with non-constant $w_{\\phi}$ and, hence, how it could be used in reconstruction from cosmological data.

  20. Nonequilibrium Dynamics of Scalar Fields in a Thermal Bath

    CERN Document Server

    Anisimov, A; Drewes, M; Mendizabal, S

    2008-01-01

    We study the approach to equilibrium for a scalar field which is coupled to a large thermal bath. Our analysis of the initial value problem is based on Kadanoff-Baym equations which are shown to be equivalent to a stochastic Langevin equation. The interaction with the thermal bath generates a temperature-dependent spectral density, either through decay and inverse decay processes or via Landau damping. In equilibrium, energy density and pressure are determined by the Bose-Einstein distribution function evaluated at a complex quasi-particle pole. The time evolution of the statistical propagator is compared with solutions of the Boltzmann equations for particles as well as quasi-particles. The dependence on initial conditions and the range of validity of the Boltzmann approximation are determined.

  1. Free box^k Scalar Conformal Field Theory

    CERN Document Server

    Brust, Christopher

    2016-01-01

    We consider the generalizations of the free U(N) and O(N) scalar conformal field theories to actions with higher powers of the Laplacian, box^k, in general dimension d. We study the spectra, Verma modules, anomalies and OPE of these theories. We argue that in certain d and k, the spectrum contains zero norm operators which are both primary and descendant, as well as extension operators which are neither primary nor descendant. In addition, we argue that in even dimensions d <= 2k, there are well-defined operator algebras which are related to the box^k theories and are novel in that they have a finite number of single-trace states.

  2. Axial, Scalar and Tensor Charges of the Nucleon from 2+1+1-flavor Lattice QCD

    CERN Document Server

    Bhattacharya, Tanmoy; Cohen, Saul; Gupta, Rajan; Lin, Huey-Wen; Yoon, Boram

    2016-01-01

    We present results for the isovector axial, scalar and tensor charges $g^{u-d}_A$, $g^{u-d}_S$ and $g^{u-d}_T$ of the nucleon needed to probe the Standard Model and novel physics. The axial charge is a fundamental parameter describing the weak interactions of nucleons. The scalar and tensor charges probe novel interactions at the TeV scale in neutron and nuclear $\\beta$-decays, and the flavor-diagonal tensor charges $g^{u}_T$, $g^{d}_T$ and $g^{s}_T$ are needed to quantify the contribution of the quark electric dipole moment (EDM) to the neutron EDM. The lattice-QCD calculations were done using nine ensembles of gauge configurations generated by the MILC Collaboration using the HISQ action with 2+1+1 dynamical flavors. These ensembles span three lattice spacings $a \\approx 0.06, 0.09$ and $0.12$ fm and light-quark masses corresponding to the pion masses $M_\\pi \\approx$ 135, 225 and 315 MeV. High-statistics estimates on five ensembles using the all-mode-averaging method allow us to quantify all systematic unce...

  3. Far Field Evolution of Momentum Driven and Scalar Dominated Flow Field

    Directory of Open Access Journals (Sweden)

    V. Ilangovan

    2016-01-01

    Full Text Available To capture the effect of initial conditions in far field evolution of momentum driven and scalar dominated flow field, Witze scaling has been used for collapsing vector and scalar data to attain asymptotic state at self-preserving region of the jet. It incorporates the initial mass, momentum, energy to capture the effect of heating level on both near and far field development of strongly heated coaxial turbulent round air jets entering into quiescent ambient. This paper compares the effectiveness of potential core length and jet effective diameter as the length scales to collapse both mean and fluctuating components of velocity vector and temperature scalar. Similarity considerations with Witze length scale using the initial momentum flux and buoyancy flux gives a good collapse at all levels of heating.

  4. Propagators of charged particles in an external magnetic field, expanded over Landau levels

    CERN Document Server

    Kuznetsov, A V; Shitova, A M

    2015-01-01

    Various forms of expressions for the propagators of charged particles in a constant magnetic field that should be used for investigations of electroweak processes in external uniform magnetic field are discussed. Formulas for the propagators of the Standard Model charged $W$- and scalar $\\Phi$-bosons in an arbitrary $\\xi$-gauge, expanded over Landau levels, are derived for the first time.

  5. Loop representation for 2-D Wilson lattice fermions in a scalar background field

    OpenAIRE

    Gattringer, Christof

    1998-01-01

    We show that the fermion determinant for 2-D Wilson lattice fermions coupled to an external scalar field is equivalent to self avoiding loops interacting with the external field. In an application of the resulting formula we integrate the scalar field with a Gaussian action to generate the N-component Gross-Neveu model. The loop representation for this model is discussed.

  6. Isovector Scalar Field Effects in Asymmetric Nuclear Matter

    Institute of Scientific and Technical Information of China (English)

    WANG Zhi-Xia; LIU Bo; ZHANG Xi-He; SHEN Cai-Wan; SHEN Ke; M. Di Toro; ZHAO En-Guang

    2008-01-01

    Density-dependent parametrization models of the nucleon-meson coupling constants, including the isovector scalar δ-field, are applied to asymmetric nuclear matter. The nuclear equation of state (EOS) and the neutron star properties are studied in a relativistic Lagrangian density, using the relativistic mean field (RMF) hadron theory. It is known that the 5-field in the constant coupling scheme leads to a larger repulsion in dense neutron-rich matter and to a definite splitting of proton and neutron effective masses, finally influences the stability of the neutron stars. We use density-dependent models of the nucleon-meson couplings to study the properties of neutron star matter and to reexamine the δ-field effects in asymmetric nuclear matter. Our calculation shows that the stability conditions of the neutron star matter can be improved in presence of the 5-meson in the density-dependent models of the coupling constants. The EOS of nuclear matter strongly depends on the density dependence of the interactions.

  7. Superfield approach to symmetry invariance in quantum electrodynamics with complex scalar fields

    Indian Academy of Sciences (India)

    R P Malik; B P Mandal

    2009-05-01

    We show that the Grassmannian independence of the super-Lagrangian density, expressed in terms of the superfields defined on a (4,2)-dimensional supermanifold, is a clear-cut proof for the Becchi–Rouet–Stora–Tyutin (BRST) and anti-BRST invariance of the corresponding four (3+1)-dimensional (4D) Lagrangian density that describes the interaction between the (1) gauge field and the charged complex scalar fields. The above 4D field theoretical model is considered on a (4,2)-dimensional supermanifold para- metrized by the ordinary four space-time variables (with = 0, 1, 2, 3) and a pair of Grassmannian variables and $\\bar{}$ (with $^{2} = \\bar{}^{2} = 0$, $\\bar{} + \\bar{} = 0$). Geometrically, the (anti-)BRST invariance is encoded in the translation of the super-Lagrangian density along the Grassmannian directions of the above supermanifold such that the outcome of this shift operation is zero.

  8. The continuous tower of scalar fields as a system of interacting dark matter–dark energy

    OpenAIRE

    Paulo Santos

    2016-01-01

    This paper aims to introduce a new parameterisation for the coupling Q in interacting dark matter and dark energy models by connecting said models with the Continuous Tower of Scalar Fields model. Based upon the existence of a dark matter and a dark energy sectors in the Continuous Tower of Scalar Fields, a simplification is considered for the evolution of a single scalar field from the tower, validated in this paper. This allows for the results obtained with the Continuous Tower of Scalar Fi...

  9. Strong field gravitational lensing by a charged Galileon black hole

    CERN Document Server

    Zhao, Shan-Shan

    2016-01-01

    Strong field gravitational lensings are dramatically disparate from those in the weak field by representing relativistic images due to light winds one to infinity loops around a lens before escaping. We study such a lensing caused by a charged Galileon black hole, which is expected to have possibility to evade no-hair theorem. We calculate the angular separations and time delays between different relativistic images of the charged Galileon black hole. All these observables can potentially be used to discriminate a charged Galileon black hole from others. We estimate the magnitudes of the observables for the closest suppermassive black hole Sgr A*. It is found that when the scalar filed in the Galileon is weakly coupled to the gravitational field and it is "low-speed", the charged Galileon black hole can possibly be distinguished from a Reissner-Nordstr\\"om black hole.

  10. Parametrized post Newtonian approximation in teleparallel model with a scalar field coupled to torsion and boundary term

    CERN Document Server

    Sadjadi, H Mohseni

    2016-01-01

    We study the parameterized post Newtonian approximation in teleparallel model of gravity with a scalar field. The scalar field is non-minimally coupled to the scalar torsion as well as to the boundary term introduced in [1]. We show that, in contrast to the case where the scalar field is only coupled to the scalar torsion, the presence of the new coupling affects the parameterized post Newtonian parameters. These parameters for different situations are obtained and discussed.

  11. Effective field theory of modified gravity with two scalar fields: dark energy and dark matter

    CERN Document Server

    Gergely, László Á

    2014-01-01

    We present a framework for discussing the cosmology of dark energy and dark matter based on two scalar degrees of freedom. An effective field theory of cosmological perturbations is employed. A unitary gauge choice renders the dark energy field into the gravitational sector, for which we adopt a generic Lagrangian depending on three-dimensional geometrical scalar quantities arising in the ADM decomposition. We add to this dark-energy associated gravitational sector a scalar field $\\phi$ and its kinetic energy $X$ as dark matter variables. Compared to the single-field case, we find that there are additional conditions to obey in order to keep the equations of motion for linear cosmological perturbations at second order. For such a second-order multi-field theory we derive conditions under which ghosts and Laplacian instabilities of the scalar and tensor perturbations are absent. We apply our general results to models with dark energy emerging in the framework of the Horndeski theory and dark matter described b...

  12. Nucleon Scalar and Tensor Charges from Lattice QCD with Light Wilson Quarks

    CERN Document Server

    Green, J R; Pochinsky, A V; Syritsyn, S N; Engelhardt, M; Krieg, S

    2012-01-01

    We present 2+1 flavor Lattice QCD calculations of the nucleon scalar and tensor charges. Using the BMW clover-improved Wilson action with pion masses between 150 and 350 MeV and three source-sink separations between 0.9 and 1.4 fm, we achieve good control over excited-state contamination and extrapolation to the physical pion mass. As a consistency check, we also present results from calculations using unitary domain wall fermions with pion masses between 300 and 400 MeV, and using domain wall valence quarks and staggered sea quarks with pion masses between 300 and 600 MeV.

  13. Singular and non-singular endstates in massless scalar field collapse

    CERN Document Server

    Bhattacharya, Swastik

    2011-01-01

    We study the collapse of a massless scalar field coupled to gravity. A class of blackhole solutions are identified. We also report on a class of solutions where collapse starts from a regular spacelike surface but then the collapsing scalar field freezes. As a result, in these solutions, a black hole does not form, neither is there any singularity in the future.

  14. Reconstruction of scalar field theories realizing inflation consistent with the Planck and BICEP2 results

    Energy Technology Data Exchange (ETDEWEB)

    Bamba, Kazuharu [Leading Graduate School Promotion Center, Ochanomizu University, 2-1-1 Ohtsuka, Bunkyo-ku, Tokyo 112-8610 (Japan); Department of Physics, Graduate School of Humanities and Sciences, Ochanomizu University, Tokyo 112-8610 (Japan); Nojiri, Shin' ichi [Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Nagoya 464-8602 (Japan); Department of Physics, Nagoya University, Nagoya 464-8602 (Japan); Odintsov, Sergei D. [Consejo Superior de Investigaciones Científicas, ICE/CSIC-IEEC, Campus UAB, Facultat de Ciències, Torre C5-Parell-2a pl, E-08193 Bellaterra (Barcelona) (Spain); Institució Catalana de Recerca i Estudis Avançats (ICREA), Barcelona (Spain); Tomsk State Pedagogical University, 634061 Tomsk (Russian Federation); National Research Tomsk State University, 634050 Tomsk (Russian Federation); King Abdulaziz University, Jeddah (Saudi Arabia)

    2014-10-07

    We reconstruct scalar field theories to realize inflation compatible with the BICEP2 result as well as the Planck. In particular, we examine the chaotic inflation model, natural (or axion) inflation model, and an inflationary model with a hyperbolic inflaton potential. We perform an explicit approach to find out a scalar field model of inflation in which any observations can be explained in principle.

  15. A flashless quantization of the scalar field on the "trousers"

    CERN Document Server

    Krasnikov, S

    2016-01-01

    The "trousers" spacetime is a pair of flat 2D cylinders ("legs") merging into into a single one ("trunk"). In spite of its simplicity this spacetime has a few features (including, in particular, a naked singularity in the "crotch") each of which is presumably unphysical, but for none of which a mechanism is known able to prevent its occurrence. Therefore it is interesting and important to study the behavior of the quantum fields in such a space. Anderson and DeWitt were the first to consider the free scalar field in the trousers spacetime. They argued that the crotch singularity produces an infinitely bright flash, which was interpreted as evidence that the topology of space is dynamically preserved. Similar divergencies were later discovered by Manogue, Copeland and Dray who used a more exotic quantization scheme. Later yet the same result obtained within a somewhat different approach led Sorkin to the conclusion that the topological transition in question is suppressed in quantum gravity. In this paper I sh...

  16. Fuzzy Scalar Field Theories: Numerical and Analytical Investigations

    CERN Document Server

    Medina, Julieta

    2006-01-01

    This thesis is devoted to the study of Quantum Field Theories (QFT) on fuzzy spaces. Fuzzy spaces are approximations to the algebra of functions of a continuous space by a finite matrix algebra. In the limit of infinitely large matrices the formulation is exact. An attractive feature of this approach is that it transparently shows how the geometrical properties of the continuous space are preserved. In the study of the non-perturbative regime of QFT, fuzzy spaces provide a possible alternative to the lattice as a regularisation method. The thesis is divided into two parts. We perform Monte Carlo simulations of a $\\lambda \\phi^4$ theory on a 3-dimensional Euclidean space. We identify the phase diagram of this model. In addition to the usual disordered and uniform ordered phases we find a third phase of non-uniform ordering. This indicates the existence of the phenomenon called UV-IR mixing in the strong coupling regime. Second we present a geometrical analysis of the scalar field theory on a 4-dimensional fuzz...

  17. Scalar Field Theories On The World Sheet: Cutoff Independent Treatment

    CERN Document Server

    Bardakci, Korkut

    2013-01-01

    Following earlier work on the same topic, we consider once more scalar field theories on the world sheet parametrized by the light cone coordinates. For most of the way, we use the same approach as in the previous work, but there is an important new development. To avoid the light cone singularity at p^{+}=0, one world sheet coordinate had to be discretized, introducing a cutoff into the model.In the earlier work, this cutoff could not be removed, making the model unreliable. In the present article, we show that, by a careful choice of the mass counter term, both the infrared singularity at p^{+}=0 and the ultraviolet mass divergences can be simultaneously eliminated. We therefore finally have a cutoff independent model on a continuously parametrized world sheet. We study this model in the mean field approximation, and as before, we find solitonic solutions. Quantizing the solitonic collective coordinates gives rise to a string like model. However, in contrast to the standard string model, the trajectories he...

  18. Axial, scalar, and tensor charges of the nucleon from 2 +1 +1 -flavor Lattice QCD

    Science.gov (United States)

    Bhattacharya, Tanmoy; Cirigliano, Vincenzo; Cohen, Saul D.; Gupta, Rajan; Lin, Huey-Wen; Yoon, Boram; Precision Neutron Decay Matrix Elements Pndme Collaboration

    2016-09-01

    We present results for the isovector axial, scalar, and tensor charges gAu -d , gSu -d, and gTu -d of the nucleon needed to probe the Standard Model and novel physics. The axial charge is a fundamental parameter describing the weak interactions of nucleons. The scalar and tensor charges probe novel interactions at the TeV scale in neutron and nuclear β -decays, and the flavor-diagonal tensor charges gTu, gTd, and gTs are needed to quantify the contribution of the quark electric dipole moment (EDM) to the neutron EDM. The lattice-QCD calculations were done using nine ensembles of gauge configurations generated by the MILC Collaboration using the highly improved staggered quarks action with 2 +1 +1 dynamical flavors. These ensembles span three lattice spacings a ≈0.06 ,0.09 , and 0.12 fm and light-quark masses corresponding to the pion masses Mπ≈135 ,225 , and 315 MeV. High-statistics estimates on five ensembles using the all-mode-averaging method allow us to quantify all systematic uncertainties and perform a simultaneous extrapolation in the lattice spacing, lattice volume, and light-quark masses for the connected contributions. Our final estimates, in the MS ¯ scheme at 2 GeV, of the isovector charges are gAu -d=1.195 (33 )(20 ) , gSu -d=0.97 (12 )(6 ), and gTu -d=0.987 (51 )(20 ) . The first error includes statistical and all systematic uncertainties except that due to the extrapolation Ansatz, which is given by the second error estimate. Combining our estimate for gSu -d with the difference of light quarks masses (md-mu)QCD=2.67 (35 ) MeV given by the Flavor Lattice Average Group, we obtain (MN-MP)QCD=2.59 (49 ) MeV . Estimates of the connected part of the flavor-diagonal tensor charges of the proton are gTu=0.792 (42 ) and gTd=-0.194 (14 ). Combining our new estimates with precision low-energy experiments, we present updated constraints on novel scalar and tensor interactions, ɛS ,T, at the TeV scale.

  19. Casimir entropy and internal energy of the objects in fluctuating scalar and electromagnetic fields

    CERN Document Server

    Jafari, Marjan

    2016-01-01

    Casimir entropy is an important aspect of casimir effect.In this paper,we employ the path integral method to derive the total relation for casimir entropy and internal energy of arbitrary shaped objects in the presence of two,three and four dimensions scalar fields and electromagnetic field.We obtain the casimir entropy and internal energy of two nanoribbon immersed in scalar field and two nanospheres immersed in scalar field and electromagnetic field.The casmir entropy of two nanospheres immersed in the electromagnetic field in small interval of temperature variations,shown a different behavior.

  20. Gravitational collapse of massless scalar field in $f(R)$ gravity

    CERN Document Server

    Zhang, Cheng-Yong; Wang, Bin

    2016-01-01

    We study the spherically symmetric gravitational collapse of massless scalar matter field in asymptotic flat spacetime in $f(R)$ gravity. In the Einstein frame of $f(R)$ gravity, an additional scalar field arises due to the conformal transformation. We find that besides the usual competition between gravitational energy and kinetic energy in the process of gravitational collapse, the new scalar field brought by the conformal transformation adds one more competing force in the dynamical system. The dynamical competition can be controlled by tuning the amplitudes of the initial perturbations of the new scalar field and the matter field. To understand the physical reasons behind these phenomena, we analyze the gravitational potential behavior and calculate the Ricci scalar at center with the change of initial amplitudes of perturbations. We find rich physics on the formation of black holes through gravitational collapse in $f(R)$ gravity.

  1. The continuous tower of scalar fields as a system of interacting dark matter–dark energy

    Directory of Open Access Journals (Sweden)

    Paulo Santos

    2015-10-01

    Full Text Available This paper aims to introduce a new parameterisation for the coupling Q in interacting dark matter and dark energy models by connecting said models with the Continuous Tower of Scalar Fields model. Based upon the existence of a dark matter and a dark energy sectors in the Continuous Tower of Scalar Fields, a simplification is considered for the evolution of a single scalar field from the tower, validated in this paper. This allows for the results obtained with the Continuous Tower of Scalar Fields model to match those of an interacting dark matter–dark energy system, considering that the energy transferred from one fluid to the other is given by the energy of the scalar fields that start oscillating at a given time, rather than considering that the energy transference depends on properties of the whole fluids that are interacting.

  2. Jacobi stability analysis of scalar field models with minimal coupling to gravity in a cosmological background

    CERN Document Server

    Dănilă, Bogdan; Mak, Man Kwong; Pantaragphong, Praiboon; Sabau, Sorin

    2016-01-01

    We perform the study of the stability of the cosmological scalar field models, by using the Jacobi stability analysis, or the Kosambi-Cartan-Chern (KCC) theory. In the KCC approach we describe the time evolution of the scalar field cosmologies in geometric terms, by performing a "second geometrization", by considering them as paths of a semispray. By introducing a non-linear connection and a Berwald type connection associated to the Friedmann and Klein-Gordon equations, five geometrical invariants can be constructed, with the second invariant giving the Jacobi stability of the cosmological model. We obtain all the relevant geometric quantities, and we formulate the condition of the Jacobi stability for scalar field cosmologies in the second order formalism. As an application of the developed methods we consider the Jacobi stability properties of the scalar fields with exponential and Higgs type potential. We find that the Universe dominated by a scalar field exponential potential is in Jacobi unstable state, ...

  3. Localization of gravity on a thick braneworld without scalar fields

    CERN Document Server

    Herrera-Aguilar, Alfredo; Mora-Luna, Refugio Rigel

    2010-01-01

    In this work we present a simple thick braneworld model that is generated by an intriguing interplay between a 5D cosmological constant with a de Sitter metric induced in the 3-brane without the inclusion of scalar fields. We show that 4D gravity is localized on this brane, provide analytic expressions for the massive Kaluza-Klein (KK) fluctuation modes and also show that the spectrum of metric excitations displays a mass gap. We finally present the corrections to Newton's law due to these massive modes. This model has no naked singularities along the fifth dimension despite the existence of a mass gap in the graviton spectrum as it happens in thick branes with 4D Poincare symmetry, providing a simple model with very good features: the curvature is completely smooth along the fifth dimension, it localizes 4D gravity and the spectrum of gravity fluctuations presents a mass gap, a fact that rules out the existence of phenomenologically dangerous ultralight KK excitations in the model.

  4. Cosmological perturbations in coherent oscillating scalar field models

    Science.gov (United States)

    Cembranos, J. A. R.; Maroto, A. L.; Jareño, S. J. Núñez

    2016-03-01

    The fact that fast oscillating homogeneous scalar fields behave as perfect fluids in average and their intrinsic isotropy have made these models very fruitful in cosmology. In this work we will analyse the perturbations dynamics in these theories assuming general power law potentials V( ϕ) = λ| ϕ| n /n. At leading order in the wavenumber expansion, a simple expression for the effective sound speed of perturbations is obtained c eff 2 = ω = ( n - 2)/( n + 2) with ω the effective equation of state. We also obtain the first order correction in k 2/ ω eff 2 , when the wavenumber k of the perturbations is much smaller than the background oscillation frequency, ω eff. For the standard massive case we have also analysed general anharmonic contributions to the effective sound speed. These results are reached through a perturbed version of the generalized virial theorem and also studying the exact system both in the super-Hubble limit, deriving the natural ansatz for δϕ; and for sub-Hubble modes, exploiting Floquet's theorem.

  5. Cosmological perturbations in coherent oscillating scalar field models

    CERN Document Server

    Cembranos, J A R; Jareño, S J Núñez

    2015-01-01

    The fact that fast oscillating homogeneous scalar fields behave as perfect fluids in average and their intrinsic isotropy have made these models very fruitful in cosmology. In this work we will analyse the perturbations dynamics in these theories assuming general power law potentials $V(\\phi)=\\lambda \\vert\\phi\\vert^{n}/n$. At leading order in the wavenumber expansion, a simple expression for the effective sound speed of perturbations is obtained $c_{\\text{eff}}^2 = \\omega=(n-2)/(n+2)$ with $\\omega$ the effective equation of state. We also obtain the first order correction in $k^2/\\omega_{\\text{eff}}^2$, when the wavenumber $k$ of the perturbations is much smaller than the background oscillation frequency, $\\omega_{\\text{eff}}$. For the standard massive case we have also analysed general anharmonic contributions to the effective sound speed. These results are reached through a perturbed version of the generalized virial theorem and also studying the exact system both in the super-Hubble limit, deriving the nat...

  6. Thermodynamics of Lovelock black holes with a nonminimal scalar field

    CERN Document Server

    Correa, Francisco

    2013-01-01

    We source the Lovelock gravity theories indexed by an integer k and fixed by requiring a unique anti-de Sitter vacuum with a self-interacting nonminimal scalar field in arbitrary dimension d. For each inequivalent Lovelock gravity theory indexed by the integer k, we establish the existence of a two-parametric self-interacting potential that permits to derive a class of black hole solutions with planar horizon for any arbitrary value of the nonminimal coupling parameter. In the thermodynamical analysis of the solution, we show that, once regularized the Euclidean action, the mass contribution coming form the gravity side exactly cancels, order by order, the one arising from the matter part yielding to a vanishing mass. This result is in accordance with the fact that the entropy of the solution, being proportional to the lapse function evaluated at the horizon, also vanishes. Consequently, the integration constant appearing in the solution is interpreted as a sort of hair which turns out to vanish at high tempe...

  7. Electric charge in the stochastic electric field

    CERN Document Server

    Simonov, Yu A

    2016-01-01

    The influence of electric stochastic fields on the relativistic charged particles is investigated in the gauge invariant path integral formalism. Using the cumulant expansion one finds the exponential relaxation of the charge Green's function both for spinless and Dirac charges.

  8. Neutron star mass-radius relation with gravitational field shielding by a scalar field

    Institute of Scientific and Technical Information of China (English)

    Bo-Jun Zhang; Tian-Xi Zhang; Padmaja Guggilla; Mostafa Dokhanian

    2013-01-01

    The currently well-developed models for equations of state (EoSs) have been severely impacted by recent measurements of neutron stars with a small radius and/or large mass.To explain these measurements,the theory of gravitational field shielding by a scalar field is applied.This theory was recently developed in accordance with the five-dimensional (5D) fully covariant Kaluza-Klein (KK) theory that has successfully unified Einstein's general relativity and Maxwell's electromagnetic theory.It is shown that a massive,compact neutron star can generate a strong scalar field,which can significantly shield or reduce its gravitational field,thus making it more massive and more compact.The mass-radius relation developed under this type of modified gravity can be consistent with these recent measurements of neutron stars.In addition,the effect of gravitational field shielding helps explain why the supernova explosions of some very massive stars (e.g.,40 M⊙ as measured recently) actually formed neutron stars rather than black holes as expected.The EoS models,ruled out by measurements of small radius and/or large mass neutron stars according to the theory of general relativity,can still work well in terms of the 5D fully covariant KK theory with a scalar field.

  9. Thermodynamics of hot quantum scalar field in a (D+1) dimensional curved spacetime

    CERN Document Server

    C., W A Rojas

    2016-01-01

    We use the brick wall model to calculate the free energy of quantum scalar field in a curved spacetime (D +1) dimensions. We find the thermodynamics properties of quantum scalar field in several scenaries: Minkowski spacetime, Schwarzschild spacetime and BTZ spacetime. For the cases analysed, the thermodynamical properties of quantum scalar field is exactly with the reported. It was found that the entropy of the gas is proportional to the horizon area in a gravity field strong, which is consistent with the holographic principle.

  10. A Riccati equation based approach to isotropic scalar field cosmologies with arbitrary self-interaction potentials

    CERN Document Server

    Harko, Tiberiu; Mak, M K

    2014-01-01

    Gravitationally coupled scalar fields $\\phi $, distinguished by the choice of an effective self-interaction potential $V(\\phi )$, simulating a temporarily non-vanishing cosmological term, can generate both inflation and late time acceleration. In scalar field cosmological models the evolution of the Hubble function is determined, in terms of the interaction potential, by a Riccati type equation. In the present work we investigate scalar field cosmological models that can be obtained as solutions of the Riccati evolution equation for the Hubble function. Four exact integrability cases of the field equations are presented, representing classes of general solutions of the Riccati evolution equation, and their cosmological properties are investigated in detail.

  11. Complex frequencies of a massless scalar field in loop quantum black hole spacetime

    Institute of Scientific and Technical Information of China (English)

    Chen Ju-Hua; Wang Yong-Jiu

    2011-01-01

    Recently, considerable progress has been made in understanding the early universe by loop quantum cosmology. Modesto et at. investigated the loop quantum black hole (LQBH)using improved semiclassical analysis and they found that the LQBH has two horizons, an event horizon and a Cauchy horizon, just like the Reissner-Nordstr(o)m black hole. This paper focuses on the dynamical evolution of a massless scalar wave in the LQBH background. By investigating the relation between the complex frequencies of the massless scalar field and the LQBH parameters using the numerical method, we find that the polymeric parameter P makes the massless scalar field decay more quickly and makes the ground scalar wave oscillate slowly. However, the polymeric parameter P causes the frequency of the high harmonic massless scalar wave to shift according to its value. We also find that the loop quantum gravity area gap parameter a0 causes the massless scalar field to decay more slowly and makes the period of the massless scalar field wave become longer. In the complex ω plane, the frequency curves move counterclockwise when the polymeric parameter P increases and this spiral effect is more obvious for a higher harmonic scalar wave.

  12. Charged and Electromagnetic Fields from Relativistic Quantum Geometry

    Directory of Open Access Journals (Sweden)

    Marcos R. A. Arcodía

    2016-06-01

    Full Text Available In the recently introduced Relativistic Quantum Geometry (RQG formalism, the possibility was explored that the variation of the tensor metric can be done in a Weylian integrable manifold using a geometric displacement, from a Riemannian to a Weylian integrable manifold, described by the dynamics of an auxiliary geometrical scalar field θ, in order that the Einstein tensor (and the Einstein equations can be represented on a Weyl-like manifold. In this framework we study jointly the dynamics of electromagnetic fields produced by quantum complex vector fields, which describes charges without charges. We demonstrate that complex fields act as a source of tetra-vector fields which describe an extended Maxwell dynamics.

  13. The two photon decay of a bound state of exotic colored scalars charged under an additional unbroken gauge interaction

    CERN Document Server

    Foot, Robert

    2016-01-01

    We argue that a charged scalar particle $\\chi$ of mass around 375 GeV charged under both $\\mathrm{SU}(3)_{c}$ and a new confining non-abelian gauge interaction can explain the 750 GeV diphoton excess. After pair production, these interactions confine the exotic scalar into non-relativistic bound states whose decays into photons can explain the discrepancy. Taking the new confining group to be $\\mathrm{SU}(2)$, we find $\\chi$ must carry an electric charge of $Q \\approx 1/2$ to fit the data. Interestingly, we find that pair production of the scalars and the subsequent formation of the bound state dominates over direct bound state resonance production. This explanation is quite weakly constrained by current experimental bounds, and we expect future constraints to come from dijet, mono-jet and possibly dilepton searches.

  14. Massive scalar field quasinormal modes of a Schwarzschild black hole surrounded by quintessence

    CERN Document Server

    Ma, C; Wang, F; Wang, W; Gui, Yuanxing; Ma, Chunrui; Wang, Fujun; Wang, Wei

    2006-01-01

    We present the quasinormal frequencies of the massive scalar field in the background of a Schwarzchild black hole surrounded by quintessence with the third-order WKB method. The mass of the scalar field $u$ plays an important role in studying the quasinormal frequencies, the real part of the frequencies increases linearly as mass $u$ increases, while the imaginary part in absolute value decreases linearly which leads to damping more slowly and the frequencies having a limited value. Moreover, owing to the presence of the quintessence, the massive scalar field damps more slowly.

  15. Transport equation for the time scale of a turbulent scalar field

    International Nuclear Information System (INIS)

    The two-parametric turbulence models cause serious difficulties by modeling the near-wall flows due to absence of the natural boundary condition on the wall for dissipation of the ε turbulence energy and the εθ scalar field destruction. This difficulty may be overcome, if instead of the ε and εθ, as the second parameter of the model, to apply the time scales of the turbulent dynamic and scalar fields. The equation of the scalar field is derived and numerical coefficients included therein, are determined from the simplest problems on the turbulent heat transfer

  16. Critical Behavior in the Gravitational Collapse of a Scalar Field with Angular Momentum in Spherical Symmetry

    OpenAIRE

    Olabarrieta, I.; Ventrella, J.; Choptuik, M.; Unruh, W.

    2007-01-01

    We study the critical collapse of a massless scalar field with angular momentum in spherical symmetry. In order to mimic the effects of angular momentum we perform a sum of the stress-energy tensors for all the scalar fields with the same eigenvalue, l, of the angular momentum operator and calculate the equations of motion for the radial part of these scalar fields. We have found that the critical solutions for different values of l are discretely self-similar (as in the original l=0 case). T...

  17. Reconstruction of the Scalar Field Potential in Inflationary Models with a Gauss-Bonnet term

    CERN Document Server

    Koh, Seoktae; Tumurtushaa, Gansukh

    2016-01-01

    We study inflationary models with a Gauss-Bonnet term to reconstruct the scalar field potentials and the Gauss-Bonnet coupling functions from the observable quantities. Using the observationally favored relations for both $n_s$ and $r$, we derive the expressions for both the scalar field potentials and the coupling functions. The implication of the blue-tilted spectrum, $n_t>0$, of the primordial tensor fluctuations is discussed for the reconstructed configurations of the scalar field potential and the Gauss-Bonnet coupling.

  18. Quantum and classical aspects of scalar and vector fields around black holes

    OpenAIRE

    Wang, Mengjie

    2016-01-01

    This thesis presents recent studies on test scalar and vector fields around black holes. It is separated in two parts according to the asymptotic properties of the spacetime under study. In the first part, we investigate scalar and Proca fields on an asymptotically flat background. For the Proca field, we obtain a complete set of equations of motion in higher dimensional spherically symmetric backgrounds. These equations are solved numerically, both to compute Hawking radiation spectra and qu...

  19. The Hamiltonian formalism for scalar fields coupled to gravity in a cosmological background

    Energy Technology Data Exchange (ETDEWEB)

    Bernardini, A.E., E-mail: alexeb@ufscar.br; Bertolami, O., E-mail: orfeu.bertolami@fc.up.pt

    2013-11-15

    A novel routine to investigate the scalar fields in a cosmological context is discussed in the framework of the Hamiltonian formalism. Starting from the Einstein–Hilbert action coupled to a Lagrangian density that contains two components–one corresponding to a scalar field Lagrangian, L{sub ϕ}, and another that depends on the scale parameter, L{sub a}–one can identify a generalized Hamiltonian density from which first-order dynamical equations can be obtained. This set up corresponds to the dynamics of Friedmann–Robertson–Walker models in the presence of homogeneous fields embedded into a generalized cosmological background fluid in a system that evolves all together isentropically. Once the generalized Hamiltonian density is properly defined, the constraints on the gravity–matter–field system are straightforwardly obtained through the first-order Hamilton equations. The procedure is illustrated for three examples of cosmological interest for studies of the dark sector: real scalar fields, tachyonic fields and generalized Born–Infeld tachyonic fields. The inclusion of some isentropic fluid component into the Friedmann equation allows for identifying an exact correspondence between the dark sector underlying scalar field and an ordinary real scalar field dynamics. As a final issue, the Hamiltonian formulation is used to set the first-order dynamical equations through which one obtains the exact analytical description of the cosmological evolution of a generalized Chaplygin gas (GCG) with dustlike matter, radiation or curvature contributions. Model stability in terms of the square of the sound velocity, c{sub s}{sup 2}, cosmic acceleration, q, and conditions for inflation are discussed. -- Highlights: •The Hamiltonian formalism for scalar fields coupled to gravity in a cosmological background is constructed. •Real scalar, tachyonic and generalized Born–Infeld tachyonic-type fields are considered. •An extended formulation of the Hamilton

  20. Casimir Effect of Massive Scalar Field with Hybrid Boundary Condition in (1+1)-Dimensional Spacetime

    Institute of Scientific and Technical Information of China (English)

    HE Xiao-Kai; LIU Wen-Biao; QIU Wei-Gang

    2009-01-01

    The Casimir energy of maesive scalar field with hybrid (Dirichlet-Neumann) boundary condition is calcu-lated. In order to regularize the model, the typical methods named as mode summation method and Green's function method are used respectively. It is found that the regularized zero-point energy density depends on the scalar field's mass. When the field is massless, the result is consistent with previous literatures.

  1. Cosmological evolution of a complex scalar field with repulsive or attractive self-interaction

    CERN Document Server

    Suárez, Abril

    2016-01-01

    We study the cosmological evolution of a complex scalar field with a self-interaction potential $V(|\\varphi|^2)$, possibly describing self-gravitating Bose-Einstein condensates, using a fully general relativistic treatment. We generalize the hydrodynamic representation of the Klein-Gordon-Einstein equations in the weak field approximation developed in our previous paper. We establish the general equations governing the evolution of a spatially homogeneous complex scalar field in an expanding background. We show how they can be simplified in the fast oscillation regime and derive the equation of state of the scalar field in parametric form for an arbitrary potential. We explicitly consider the case of a quartic potential with repulsive or attractive self-interaction and determine the phase diagram of the scalar field. We show that the transition between the weakly self-interacting regime and the strongly self-interacting regime depends on how the scattering length of the bosons compares with their effective Sc...

  2. Electroweakly interacting scalar and gauge bosons, and leptons, from field equations on spin 5+1 dimensional space

    CERN Document Server

    Besprosvany, J

    2002-01-01

    Unification ideas motivate the formulation of field equations on an extended spin space. Demanding that the Poincare symmetry be maintained, one derives scalar symmetries that are associated with flavor and gauge groups. Boson and fermion solutions are obtained with a fixed representation. A field theory can be equivalently written and interpreted in terms of elements of such space and is similarly constrained. At 5+1 dimensions, one obtains isospin and hypercharge SU(2)_L X U(1) symmetries, their vector carriers, two-flavor charged and chargeless leptons, and scalar particles. Mass terms produce breaking of the symmetry to an electromagnetic U(1), a Weinberg's angle with sin^2(theta_W)=.25, and additional information on the respective coupling constants. Their underlying spin symmetry gives information on the particles' masses; one reproduces the standard-model ratio M_Z/M_W, and predicts a Higgs mass of M_H ~114 GeV, at tree level.

  3. Scalar Perturbations on the background of Linearly and Nonlinearly Charged BTZ Black Holes

    CERN Document Server

    Tang, Zi-Yu; Zangeneh, Mahdi Kord; Wang, Bin; Saavedra, Joel

    2016-01-01

    We investigate the spacetime properties of BTZ black holes in Maxwell field and BornInfeld field and find rich properties in the spacetime structures when the model parameters vary. Employing the Landau-Lifshitz theory, we examine the thermodynamical phase transition in the charged BTZ holes. We further study the dynamical perturbation in the background of the charged BTZ black holes and find different properties of dynamical perturbations for the extreme and nonextreme charged BTZ black holes, which can serve as a new physical signal to indicate the phase transition between them.

  4. A unified optical theorem for scalar and vectorial wave fields

    NARCIS (Netherlands)

    Wapenaar, C.P.A.; Douma, H.

    2012-01-01

    The generalized optical theorem is an integral relation for the angle-dependent scattering amplitude of an inhomogeneous scattering object embedded in a homogeneous background. It has been derived separately for several scalar and vectorial wave phenomena. Here a unified optical theorem is derived t

  5. One-loop omega-potential of charged massive fields in a constant homogeneous magnetic field at high temperatures

    CERN Document Server

    Kalinichenko, I S

    2016-01-01

    The explicit expressions for the high-temperature expansions of the one-loop corrections to the omega-potential coming from the charged scalar and Dirac particles and, separately, from antiparticles in a constant homogeneous magnetic field are derived. The explicit expressions for the non-perturbative corrections to the effective action at finite temperature and density are obtained. The thermodynamic properties of a gas of charged scalars in a constant homogeneous magnetic field are analyzed in the one-loop approximation. It turns out that, in this approximation, the system suffers the first order phase transition from the diamagnetic to the superconducting state at sufficiently high densities. The improvement of the one-loop result by summing the ring diagrams is investigated. This improvement leads to a drastic change of the thermodynamic properties of the system. The gas of charged scalars passes to the ferromagnetic state in place of the superconducting one at high densities and sufficiently low temperat...

  6. Quasi-stationary solutions of self-gravitating scalar fields around black holes

    CERN Document Server

    Sanchis-Gual, Nicolas; Montero, Pedro J; Font, José A

    2014-01-01

    Recent perturbative studies have shown the existence of long-lived, quasi-stationary configurations of scalar fields around black holes. In particular, such configurations have been found to survive for cosmological timescales, which is a requirement for viable dark matter halo models in galaxies based on such type of structures. In this paper we perform a series of numerical relativity simulations of dynamical non-rotating black holes surrounded by self-gravitating scalar fields. We solve numerically the coupled system of equations formed by the Einstein and the Klein-Gordon equations under the assumption of spherical symmetry using spherical coordinates. Our results confirm the existence of oscillating, long-lived, self-gravitating scalar fields configurations around non-rotating black holes in highly dynamical spacetimes with a rich scalar field environment. Our numerical simulations are long-term stable and allow for the extraction of the resonant frequencies to make a direct comparison with results obtai...

  7. Correspondence of f(R,∇R) Modified Gravity with Scalar Field Models

    International Nuclear Information System (INIS)

    This paper is devoted to study the scalar field dark energy models by taking its different aspects in the framework of f(R,∇R) gravity. We consider flat FRW universe to construct the equation of state parameter governed by f(R,∇R) gravity. The stability of the model is discussed with the help of squared speed of sound parameter. It is found that models show quintessence behavior of the universe in stable as well as unstable modes. We also develop the correspondence of f(R,∇R) model with some scalar field dark energy models like quintessence, tachyonic field, k-essence, dilaton, hessence, and DBI-essence. The nature of scalar fields and corresponding scalar potentials is being analyzed in f(R,∇R) gravity graphically which show consistency with the present day observations about accelerated phenomenon

  8. New class of cosmological solutions for a self-interacting scalar field

    Science.gov (United States)

    Chaadaev, A. A.; Chervon, S. V.

    2013-12-01

    New cosmological solutions are found to the system of Einstein scalar field equations using the scalar field φ as the argument. For a homogeneous and isotropic Universe, the system of equations is reduced to two equations, one of which is an equation of Hamilton-Jacobi type. Using the hyperbolically parameterized representation of this equation together with the consistency condition, explicit dependences of the potential V of the scalar field and the Hubble parameter H on φ are obtained. The dependences of the scalar field and the scale factor a on cosmic time t have also been found. It is shown that this scenario corresponds to the evolution of the Universe with accelerated expansion out to times distant from the initial singularity.

  9. On localization of universal scalar fields in a tachyonic de Sitter thick braneworld

    CERN Document Server

    Diaz-Furlong, Alfonso; Linares, Roman; Mora-Luna, Refugio Rigel; Morales-Tecotl, Hugo A

    2014-01-01

    Braneworld models may yield interesting effects ranging from high-energy physics to cosmology, or even some low-energy physics. Their mode structure modifies standard results in these physical realms that can be tested and used to set bounds on the models parameters. Now, to define braneworld deviations from standard 4D physics, a notion of matter and gravity localization on the brane is crucial. In this work we investigate the localization of universal massive scalar fields in a de Sitter thick tachyonic braneworld generated by gravity coupled to a tachyonic bulk scalar field. This braneworld possesses a 4D de Sitter induced metric and is asymptotically flat despite the presence of a negative bulk cosmological constant, a novel and interesting peculiarity that contrasts with previously known models. Universal scalar fields can be localized in this expanding braneworld if their bulk mass obeys an upper bound, otherwise they delocalize: The dynamics of the scalar field is governed by a Schroedinger equation wi...

  10. A generalisation of classical electrodynamics for the prediction of scalar field effects

    CERN Document Server

    van Vlaenderen, K J

    2003-01-01

    Within the framework of Classical Electrodynamics (CED) it is common practice to choose freely an arbitrary gauge condition with respect to a gauge transformation of the electromagnetic potentials. The Lorenz gauge condition allows for the derivation of the inhomogeneous potential wave equations (IPWE), but this also means that scalar derivatives of the electromagnetic potentials are considered to be \\emph{unphysical}. However, these scalar expressions might have the meaning of a new physical field, $\\mathsf S$. If this is the case, then a generalised CED is required such that scalar field effects are predicted and such that experiments can be performed in order to verify or falsify this generalised CED. The IPWE are viewed as a generalised Gauss law and a generalised Ampe\\`re law, that also contain derivatives of $\\mathsf S$, after reformulating the IPWE in terms of fields. Some recent experiment show positive results that are in qualitative agreement with the presented predictions of scalar field effects, b...

  11. Quasistationary solutions of self-gravitating scalar fields around collapsing stars

    CERN Document Server

    Sanchis-Gual, Nicolas; Montero, Pedro J; Font, José A; Mewes, Vassilios

    2015-01-01

    Recent work has shown that scalar fields around black holes can form long-lived, quasistationary configurations surviving for cosmological timescales. With this requirement, scalar fields cannot be discarded as viable candidates for dark matter halo models in galaxies around central supermassive black holes (SMBH). One hypothesis for the formation of most SMBHs at high redshift is the gravitational collapse of supermassive stars (SMS) with masses of $\\sim10^5 \\rm {M_{\\odot}}$. Therefore, a constraint for the existence of quasi-bound states of scalar fields is their survival to such dynamic events. To answer this question we present in this paper the results of a series of numerical relativity simulations of gravitationally collapsing, spherically symmetric stars surrounded by self-gravitating scalar fields. We use an ideal fluid equation of state with adiabatic index $\\Gamma=4/3$ which is adequate to simulate radiation-dominated isentropic SMSs. Our results confirm the existence of oscillating, long-lived, se...

  12. Perturbative self-interacting scalar field theory: a differential equation approach

    CERN Document Server

    Rocha, R; Coimbra-Araujo, C H

    2005-01-01

    We revisit the investigation about the partition function related to a \\phi^4-scalar field theory on a n-dimensional Minkowski spacetime, which is shown to be a self-interacting scalar field theory at least in 4-dimensional Minkowski spacetime. After rederiving the analytical calculation of the perturbative expansion coefficients and also the approximate values for suitable limits using Stirling's formulae, which consists of Witten's proposed questions, solved by P. Deligne, D. Freed, L. Jeffrey, and S. Wu, we investigate a spherically symmetric scalar field in a n-dimensional Minkowski spacetime. For the first perturbative expansion coefficient it is shown how it can be derived a modified Bessel equation (MBE), which solutions are investigated in one, four, and eleven-dimensional Minkowski spacetime. The solutions of MBE are the first expansion coefficient of the series associated with the partition function of \\phi^4-scalar field theory.

  13. Scalar fields in Kasner-type space-times: Time dependent vacuum expectation values

    International Nuclear Information System (INIS)

    Non-constant vacuum expectation values of scalar fields in curved space-times generate important physical consequences. It is here shown this to be the case for a class of spatially homogeneous and anisotropic metrics. (Author)

  14. Entropy-corrected holographic scalar field models of dark energy in Kaluza-Klein universe

    Science.gov (United States)

    Sharif, M.; Jawad, Abdul

    2013-12-01

    We investigate the evolution of interacting holographic dark energy with logarithmic corrections in the flat Kaluza-Klein universe. We evaluate the equation of state parameter and also reconstruct the scalar field models in this scenario. For this purpose, the well-known choice of scale factor in the power law form is taken. It is interesting to mention here that the corresponding equation of state parameter crosses the phantom divide line for a particular choice of interacting parameters. Finally, we conclude that the behavior of the dynamical scalar field as well as the scalar potential is consistent with the present observations.

  15. Exact solutions for scalar field cosmology in f(R) gravity

    CERN Document Server

    Maharaj, S D; Chervon, S V; Nikolaev, A V

    2016-01-01

    We look for exact solutions in scalar field cosmology. To achieve this we use $f(R)$ modified gravity with a scalar field and do not specify the the form of the $f(R)$ function. In particular, we study Friedmann universe assuming that acceleration of the scalar curvature is negligible. We first present solutions for special cases and then the general solution. Using initial conditions which represent the universe at the present epoch, we evaluated the constants of integration. This allows for the comparison of the scale factor in the new solutions with that of the $\\Lambda CDM$ solution, thereby affecting the age of the universe in $f(R)$ gravity.

  16. Motion of a scalar field coupled to a Yang Mills field reformulated locally with some gauge invariant variables

    CERN Document Server

    Chopin, E

    2000-01-01

    We show how to reformulate gauge theories coupled to scalar fields in terms of explicitly gauge-invariant variables. We show in the case of scalar QED that the classical theory can be reformulated in this way. We discuss the form of some realistic asymptotic solutions of these equations. The equations of motion are then also reformulated in the non-abelian case.

  17. Interacting entropy-corrected holographic scalar field models in non-flat universe

    CERN Document Server

    Khodam-Mohammadi, A

    2010-01-01

    we establish the correspondence between the tachyon, K-essence and dilaton scalar field models with the interacting entropy-corrected holographic dark energy model (ECHDE) in non-flat FRW universe. We reconstruct the potentials and the dynamics of these scalar fields according to the evolutionary behavior of the interacting ECHDE model. The results of interacting ECHDE model reduce to those obtained from the limiting case HDE without entropy-correction.

  18. Formation of Schwarzschild black hole from the scalar field collapse in four-dimensions

    CERN Document Server

    Oliveira-Neto, G

    2003-01-01

    We obtain a new self-similar solution to the Einstein's equations in four-dimensions, representing the collapse of a spherically symmetric, minimally coupled, massless, scalar field. Depending on the value of certain parameters, this solution represents the formation of naked singularities and black holes. Since the black holes are identified as the Schwarzschild ones, one may naturally see how these black holes are produced as remnants of the scalar field collapse.

  19. QCD phase transition with a power law chameleon scalar field in the bulk

    OpenAIRE

    Golanbari, T.; Mohammadi, A.; Saaidi, Kh.

    2014-01-01

    In this work, a brane world model with a perfect fluid on brane and a scalar field on bulk has been used to study quark-hadron phase transition. The bulk scalar field has an interaction with brane matter. This interaction comes into non-conservation relation which describe an energy transfer between bulk and brane. Since quark-hadron transition curly depends on the form of evolution equations therefore modification of energy conservation equation and Friedmann equation comes into some interes...

  20. Reconstruction of scalar field theories realizing inflation consistent with the Planck and BICEP2 results

    Directory of Open Access Journals (Sweden)

    Kazuharu Bamba

    2014-10-01

    Full Text Available We reconstruct scalar field theories to realize inflation compatible with the BICEP2 result as well as the Planck. In particular, we examine the chaotic inflation model, natural (or axion inflation model, and an inflationary model with a hyperbolic inflaton potential. We perform an explicit approach to find out a scalar field model of inflation in which any observations can be explained in principle.

  1. Genericity of blackhole formation in the gravitational collapse of homogeneous self-interacting scalar fields

    CERN Document Server

    Giambó, R; Magli, G

    2008-01-01

    The gravitational collapse of a wide class of self-interacting homogeneous scalar fields models is analyzed. The class is characterized by certain general conditions on the scalar field potential, which, in particular, include both asymptotically polynomial and exponential behaviors. Within this class, we show that the generic evolution is always divergent in a finite time, and then make use of this result to construct radiating star models of the Vaidya type. It turns out that blackholes are generically formed in such models.

  2. Symmetry breaking and restoration for interacting scalar and gauge fields in Lifshitz type theories

    Science.gov (United States)

    Farakos, K.; Metaxas, D.

    2012-05-01

    We consider the one-loop effective potential at zero and finite temperature in field theories with anisotropic space-time scaling, with critical exponent z = 2, including both scalar and gauge fields. Depending on the relative strength of the coupling constants for the gauge and scalar interactions, we find that there is a symmetry breaking term induced at one loop at zero temperature and we find symmetry restoration through a first-order phase transition at high temperature.

  3. Symmetry breaking and restoration for interacting scalar and gauge fields in Lifshitz type theories

    CERN Document Server

    Farakos, K

    2011-01-01

    We consider the one-loop effective potential at zero and finite temperature in field theories with anisotropic space-time scaling, with critical exponent $z=2$, including both scalar and gauge fields. Depending on the relative strength of the coupling constants for the gauge and scalar interactions, we find that there is a symmetry breaking term induced at one-loop at zero temperature and we find symmetry restoration through a first-order phase transition at high temperature.

  4. Symmetry breaking and restoration for interacting scalar and gauge fields in Lifshitz type theories

    Energy Technology Data Exchange (ETDEWEB)

    Farakos, K., E-mail: kfarakos@central.ntua.gr [Department of Physics, National Technical University of Athens, Zografou Campus, 15780 Athens (Greece); Metaxas, D., E-mail: metaxas@central.ntua.gr [Department of Physics, National Technical University of Athens, Zografou Campus, 15780 Athens (Greece)

    2012-05-01

    We consider the one-loop effective potential at zero and finite temperature in field theories with anisotropic space-time scaling, with critical exponent z=2, including both scalar and gauge fields. Depending on the relative strength of the coupling constants for the gauge and scalar interactions, we find that there is a symmetry breaking term induced at one loop at zero temperature and we find symmetry restoration through a first-order phase transition at high temperature.

  5. Note on the thermodynamics and the speed of sound of a scalar field

    CERN Document Server

    Piattella, Oliver F; Bilić, Neven

    2014-01-01

    We investigate the correspondence between a perfect fluid and a scalar field and show a possible way of expressing thermodynamic quantities such as entropy, particle number density, temperature and chemical potential in terms of the scalar field phi and its kinetic term X. We prove a theorem which relates isentropy with purely kinetic Lagrangian. As an application, we study the evolution of the gravitational potential in cosmological perturbation theory.

  6. Wheeler-DeWitt equation and Lie symmetries in Bianchi scalar-field cosmology

    Energy Technology Data Exchange (ETDEWEB)

    Paliathanasis, A. [Universidad Austral de Chile, Instituto de Ciencias Fisicas y Matematicas, Valdivia (Chile); Karpathopoulos, L. [University of Athens, Faculty of Physics, Department of Astronomy-Astrophysics-Mechanics, Athens (Greece); Wojnar, A. [Institute for Theoretical Physics, Wroclaw (Poland); Universita' di Napoli Federico II, Complesso Universitario di Monte S. Angelo, Dipartimento di Fisica ' ' E. Pancini' ' , Naples (Italy); Complesso Universitario di Monte S. Angelo, Naples (Italy); Istituto Nazionale di Fisica Nucleare (INFN) Sez. di Napoli, Naples (Italy); Capozziello, S. [Universita' di Napoli Federico II, Complesso Universitario di Monte S. Angelo, Dipartimento di Fisica ' ' E. Pancini' ' , Naples (Italy); Complesso Universitario di Monte S. Angelo, Naples (Italy); Gran Sasso Science Institute (INFN), L' Aquila (Italy); Istituto Nazionale di Fisica Nucleare (INFN) Sez. di Napoli, Naples (Italy)

    2016-04-15

    Lie symmetries are discussed for the Wheeler-De Witt equation in Bianchi Class A cosmologies. In particular, we consider general relativity, minimally coupled scalar-field gravity and hybrid gravity as paradigmatic examples of the approach. Several invariant solutions are determined and classified according to the form of the scalar-field potential. The approach gives rise to a suitable method to select classical solutions and it is based on the first principle of the existence of symmetries. (orig.)

  7. Evolution of spherical over-densities in tachyon scalar field model

    CERN Document Server

    Setare, M R; Darabi, F

    2016-01-01

    We study the tachyon scalar field model in flat FRW cosmology with the scale factor behavior $a(t)=t^n$. We consider the spherical collapse model and investigate the effects of the tachyon scalar field on the structure formation in flat FRW universe. We calculate $\\delta_{c}(z_{c})$, $\\lambda(z_{c})$, $\\xi(z_{c})$, $\\Delta_{V}(z_{c})$, $\\log [\

  8. Quasistationary solutions of self-gravitating scalar fields around collapsing stars

    Science.gov (United States)

    Sanchis-Gual, Nicolas; Degollado, Juan Carlos; Montero, Pedro J.; Font, José A.; Mewes, Vassilios

    2015-10-01

    Recent work has shown that scalar fields around black holes can form long-lived, quasistationary configurations surviving for cosmological time scales. Scalar fields thus cannot be discarded as viable candidates for dark matter halo models in galaxies around central supermassive black holes (SMBHs). One hypothesized formation scenario of most SMBHs at high redshift is the gravitational collapse of supermassive stars (SMSs) with masses of ˜105 M⊙ . Any such scalar field configurations must survive the gravitational collapse of a SMS in order to be a viable model of physical reality. To check for the postcollapse survival of these configurations and to follow the dynamics of the black hole-scalar field system we present in this paper the results of a series of numerical relativity simulations of gravitationally collapsing, spherically symmetric stars surrounded by self-gravitating scalar fields. We use an ideal fluid equation of state with adiabatic index Γ =4 /3 which is adequate to simulate radiation-dominated isentropic SMSs. Our results confirm the existence of oscillating, long-lived, self-gravitating scalar field configurations around nonrotating black holes after the collapse of the stars.

  9. Cosmological variation of the fine structure constant from an ultralight scalar field: The effects of mass

    Science.gov (United States)

    Gardner, Carl L.

    2003-08-01

    Cosmological variation of the fine structure constant α due to the evolution of a spatially homogeneous ultralight scalar field (m˜H0) during the matter and Λ dominated eras is analyzed. Agreement of Δα/α with the value suggested by recent observations of quasar absorption lines is obtained by adjusting a single parameter, the coupling of the scalar field to matter. Asymptotically α(t) in this model goes to a constant value α¯≈α0 in the early radiation and the late Λ dominated eras. The coupling of the scalar field to (nonrelativistic) matter drives α slightly away from α¯ in the epochs when the density of matter is important. Simultaneous agreement with the more restrictive bounds on the variation |Δα/α| from the Oklo natural fission reactor and from meteorite samples can be achieved if the mass of the scalar field is on the order of 0.5 0.6 HΛ, where HΛ=Ω1/2ΛH0. Depending on the scalar field mass, α may be slightly smaller or larger than α0 at the times of big bang nucleosynthesis, the emission of the cosmic microwave background, the formation of early solar system meteorites, and the Oklo reactor. The effects on the evolution of α due to nonzero mass for the scalar field are emphasized. An order of magnitude improvement in the laboratory technique could lead to a detection of (α˙/α)0.

  10. An Electromagnetic Form Factor of a Charged Scalar Meson with Schwinger-Dyson and Bethe-Salpeter Equations

    Institute of Scientific and Technical Information of China (English)

    XIE Chuan-Mei; LI Heng-Mei; WAN Shao-Long

    2009-01-01

    The wave functions and electromagnetic form factor of charged scalar mesons are studied with a modified vector-vector flat-bottom potential model under the framework of the Schwinger-Dyeon and Bethe-Salpeter equations.The obtained results agree well with other theories.

  11. Reconstructing the Universe Evolution from Loop Quantum Cosmology Scalar Fields

    CERN Document Server

    Oikonomou, V K

    2016-01-01

    We extend the scalar-tensor reconstruction techniques for classical cosmology frameworks, in the context of loop quantum cosmology. After presenting in some detail how the equations are generalized in the loop quantum cosmology case, we discuss which new features and limitations does the quantum framework brings along, and we use various illustrative examples in order to demonstrate how the method works. As we show the energy density has two different classes of solutions, and one of these yields the correct classical limit while the second captures the quantum phenomena. We study in detail the scalar tensor reconstruction method for both these solutions. Also we discuss some scenarios for which the Hubble rate becomes unbounded at finite time, which corresponds for example in a case that a Big Rip occurs. As we show this issue is non-trivial and we discuss how this case should be treated in a consistent way. Finally, we investigate how the classical stability conditions for the scalar-tensor solutions are ge...

  12. Effective theory of a doubly charged singlet scalar: complementarity of neutrino physics and the LHC

    CERN Document Server

    King, Stephen F; Panizzi, Luca

    2014-01-01

    We consider a rather minimal extension of the Standard Model involving just one extra particle, namely a single $SU(2)_L$ singlet scalar $S^{++}$ and its antiparticle $S^{--}$. We propose a model independent effective operator, which yields an effective coupling of $S^{\\pm \\pm}$ to pairs of same sign weak gauge bosons, $W^{\\pm} W^{\\pm}$. We also allow tree-level couplings of $S^{\\pm \\pm}$ to pairs of same sign right-handed charged leptons $l^{\\pm}_Rl'^{\\pm}_R$ of the same or different flavour. We calculate explicitly the resulting two-loop diagrams in the effective theory responsible for neutrino mass and mixing. We propose sets of benchmark points for various $S^{\\pm \\pm}$ masses and couplings which can yield successful neutrino masses and mixing, consistent with limits on charged lepton flavour violation (LFV) and neutrinoless double beta decay. We discuss the prospects for $S^{\\pm \\pm}$ discovery at the LHC, for these benchmark points, including single and pair production and decay into same sign leptons p...

  13. Rapidly rotating neutron stars with a massive scalar field - structure and universal relations

    CERN Document Server

    Doneva, Daniela D

    2016-01-01

    We construct rapidly rotating neutron star models in scalar-tensor theories with a massive scalar field. The fact that the scalar field has nonzero mass leads to very interesting results since the allowed range of values of the coupling parameters is significantly broadened. These deviations from pure general relativity can be very large for values of the parameters that are in agreement with the observations. The rapid rotation can magnify the differences several times compared to the static case. The universal relations between the normalized moment of inertia and quadrupole moment are also investigated both for the slowly and rapidly rotating cases. The results show that these relations are still EOS independent up to a large extend and the deviations from pure general relativity can be large. This places the massive scalar-tensor theories amongst the few alternative theories of gravity that can be tested via the universal $I$-Love-$Q$ relations.

  14. Inflationary universe in a conformally-invariant two scalar-field theory with an $R^2$ term

    CERN Document Server

    Bamba, Kazuharu

    2016-01-01

    We investigate the inflationary universe in a theory where two scalar fields non-minimally coupling to the scalar curvature and an extra $R^2$ term exist and the conformal invariance is broken. In particular, the slow-roll inflation is explored for the case that one scalar field is dynamical and that two scalar fields are dynamical. As a result, we show that the spectral index of the curvature perturbations and the tensor-to-scalar ratio of the density perturbations can be compatible with the Planck results. It is also demonstrated that the graceful exit from inflation can be realized.

  15. Search for charged scalars in e+e- annihilation up to 64 GeV CM energy

    International Nuclear Information System (INIS)

    A search for the production of charged scalars has been carried out in e+e- annihilation at center of mass energies up to 64 GeV with 61.1 pb-1 of integrated luminosity using the VENUS detector at TRISTAN. The assumptions concerning the production and decay of hypothetical charged scalars are minimal; they are expected to be singly charged and decay into a pair of fermions. No positive evidence for their production has been found in a study of all combinations of the anti lν(lanti ν) and Uanti D(anti UD) decay channels. We have excluded the mass region of 8.0-20.0 GeV/c2 regardless of the decay mode. (orig.)

  16. Search for charged scalars in e sup + e sup - annihilation up to 64 GeV CM energy

    Energy Technology Data Exchange (ETDEWEB)

    Yuzuki, T.; Haba, J.; Kanda, N.; Nagashima, Y.; Sugimoto, S.; Suzuki, A.; Takaki, H.; Takita, M. (Dept. of Physics, Osaka Univ., Toyonaka (Japan)); Abe, K. (Dept. of Physics, Tohoku Univ., Sendai (Japan)); Amako, K.; Arai, Y.; Fukawa, M.; Fukushima, Y.; Ishihara, N.; Kamitani, T.; Kanematsu, N.; Kanzaki, J.; Kondo, T.; Korhonen, T.T.; MacNaughton, J.; Matsui, T.; Odaka, S.; Ogawa, K.; Ohama, T.; Sakamoto, H.; Sakuda, M.; Shirai, J.; Sumiyoshi, T.; Takasaki, F.; Tsuboyama, T.; Uehara, S.; Unno, Y.; Watase, Y.; Yamada, Y. (KEK, National Lab. for High Energy Physics, Ibaraki (Japan)); Asano, Y.; Mori, S.; Shirakata, M.; Takada, Y.; Yonezawa, Y. (Inst. of Applied Physics, Univ. of Tsukuba, Ibaraki (Japan)); Chiba, M.; Fukui, T.; Hinode, F.; Hirose, T.; Minami, M.; Narita, Y.; Oyama, T.; Utsumi, M.; Watanabe, T.; Yabuki, F. (Dept. of Physics, Tokyo Metropolitan Univ. (Japan)); Chiba, Y.; Ohsugi, T.; Taketani, A.; Terunuma, N. (Dept. of Physics, Hiroshima Univ. (Japan)); Daigo, M. (Wak

    1991-09-12

    A search for the production of charged scalars has been carried out in e{sup +}e{sup -} annihilation at center of mass energies up to 64 GeV with 61.1 pb{sup -1} of integrated luminosity using the VENUS detector at TRISTAN. The assumptions concerning the production and decay of hypothetical charged scalars are minimal; they are expected to be singly charged and decay into a pair of fermions. No positive evidence for their production has been found in a study of all combinations of the anti l{nu}(lanti {nu}) and Uanti D(anti UD) decay channels. We have excluded the mass region of 8.0-20.0 GeV/c{sup 2} regardless of the decay mode. (orig.).

  17. Quantum Charged Fields in (1+1) Rindler Space

    Science.gov (United States)

    Gabriel, Cl.; Spindel, Ph.

    2000-09-01

    We study, using Rindler coordinates, the quantization of a charged scalar field interacting with a constant (Poincaré invariant), external, electric field in (1+1) dimensionnal flatspace: our main motivation is pedagogy. We illustrate in this framework the equivalence between various approaches to field quantization commonly used in the framework of curved backgrounds. First we establish the expression of the Schwinger vacuum decay rate, using the operator formalism. Then we rederive it in the framework of the Feynman path integral method. Our analysis reinforces the conjecture which identifies the zero winding sector of the Minkowski propagator with the Rindler propagator. Moreover, we compute the expression of the Unruh's modes that allow us to make a connection between the Minkowskian and Rindlerian quantization schemes by purely algebraic relations. We use these modes to study the physics of a charged two level detector moving in an electric field whose transitions are due to the exchange of charged quanta. In the limit where the Schwinger pair production mechanism of the exchanged quanta becomes negligible we recover the Boltzman equilibrium ratio for the population of the levels of the detector. Finally we explicitly show how the detector can be taken as the large mass and charge limit of an interacting fields system.

  18. The entropy of isolated horizons in non-minimally coupling scalar field theory from BF theory

    CERN Document Server

    Wang, Jingbo

    2015-01-01

    In this paper, the entropy of isolated horizons in non-minimally coupling scalar field theory and in the scalar-tensor theory of gravitation is calculated by counting the degree of freedom of quantum states in loop quantum gravity. Instead of boundary Chern-Simons theory, the boundary BF theory is used. The advantages of the new approaches are that no spherical symmetry is needed, and that the final result matches exactly with the Wald entropy formula.

  19. Scalar-field quintessence by cosmic shear: CFHT data analysis and forecasts for DUNE

    CERN Document Server

    Schimd, C; Schimd, Carlo; Tereno, Ismael

    2006-01-01

    A light scalar field, minimally or not-minimally coupled to the metric field, is a well-defined candidate for the dark energy, overcoming the coincidence problem intrinsic to the cosmological constant and avoiding the difficulties of parameterizations. We present a general description of the weak gravitational lensing valid for every metric theory of gravity, including vector and tensor perturbations for a non-flat spatial metric. Based on this description, we investigate two minimally-coupled scalar field quintessence models using VIRMOS-Descart and CFHTLS cosmic shear data, and forecast the constraints for the proposed space-borne wide-field imager DUNE.

  20. Dark Energy as a Cosmological Consequence of Existence of the Dirac Scalar Field in Nature

    Directory of Open Access Journals (Sweden)

    O. V. Babourova

    2015-01-01

    Full Text Available The solution of the field equations of the conformal theory of gravitation with Dirac scalar field in Cartan-Weyl spacetime at the very early Universe is obtained. In this theory dark energy (described by an effective cosmological constant is a function of the Dirac scalar field β. This solution describes the exponential decreasing of β at the inflation stage and has a limit to a constant value of the dark energy at large time. This can give a way to solving the fundamental cosmological constant problem as a consequence of the fields dynamics in the early Universe.

  1. Relativistic n-body wave equations in scalar quantum field theory

    Energy Technology Data Exchange (ETDEWEB)

    Emami-Razavi, Mohsen [Centre for Research in Earth and Space Science, York University, Toronto, Ontario, M3J 1P3 (Canada)]. E-mail: mohsen@yorku.ca

    2006-09-21

    The variational method in a reformulated Hamiltonian formalism of Quantum Field Theory (QFT) is used to derive relativistic n-body wave equations for scalar particles (bosons) interacting via a massive or massless mediating scalar field (the scalar Yukawa model). Simple Fock-space variational trial states are used to derive relativistic n-body wave equations. The equations are shown to have the Schroedinger non-relativistic limits, with Coulombic interparticle potentials in the case of a massless mediating field and Yukawa interparticle potentials in the case of a massive mediating field. Some examples of approximate ground state solutions of the n-body relativistic equations are obtained for various strengths of coupling, for both massive and massless mediating fields.

  2. A Viable Cosmology with a Scalar Field Coupled to the Trace of the Stress-Tensor

    CERN Document Server

    Sami, M

    2003-01-01

    We study the cosmological evolution of a scalar field that couples to the trace $T=T^{a}_a$ of energy momentum tensor of all the fields (including itself). In the case of a shallow exponential potential, the presence of coupling to the trace $T$ in the field equation makes the energy density of the scalar field decrease faster thereby hastening the commencement of radiation domination. This effect gradually diminishes at later epochs allowing the scalar field to dominate the energy density again. We interpret this phase as the current epoch of cosmic acceleration with $\\Omega_{\\phi}=0.7$. A variant of this model can lead to accelerated expansion at the present epoch followed by a $a(t)\\propto t^{2/3}$ behaviour as $t\\to \\infty$, making the model free from future event horizon. The main features of the model are independent of initial conditions. However, fine tuning of parameters is necessary for viable evolution.

  3. Inflation in a conformally invariant two-scalar-field theory with an extra R{sup 2} term

    Energy Technology Data Exchange (ETDEWEB)

    Bamba, Kazuharu, E-mail: bamba@sss.fukushima-u.ac.jp [Division of Human Support System, Faculty of Symbiotic Systems Science, Fukushima University, 960-1296, Fukushima (Japan); Leading Graduate School Promotion Center, Ochanomizu University, 112-8610, Tokyo (Japan); Department of Physics, Graduate School of Humanities and Sciences, Ochanomizu University, 112-8610, Tokyo (Japan); Odintsov, Sergei D. [Institut de Ciencies de lEspai (IEEC-CSIC), Campus UAB, Carrer de Can Magrans, s/n 08193 Cerdanyola del Valles, Barcelona (Spain); Institució Catalana de Recerca i Estudis Avançats (ICREA), Passeig Lluís Companys 23, 08010, Barcelona (Spain); Tretyakov, Petr V. [Joined Institute for Nuclear Research, Dubna, Moscow Region (Russian Federation)

    2015-07-23

    We explore inflationary cosmology in a theory where there are two scalar fields which non-minimally couple to the Ricci scalar and an additional R{sup 2} term, which breaks the conformal invariance. Particularly, we investigate the slow-roll inflation in the case of one dynamical scalar field and that of two dynamical scalar fields. It is explicitly demonstrated that the spectral index of the scalar mode of the density perturbations and the tensor-to-scalar ratio can be consistent with the observations obtaind by the recent Planck satellite. The graceful exit from the inflationary stage is achieved as in convenient R{sup 2} gravity. We also propose the generalization of the model under discussion with three scalar fields.

  4. Inflation in a conformally invariant two-scalar-field theory with an extra R{sup 2} term

    Energy Technology Data Exchange (ETDEWEB)

    Bamba, Kazuharu [Fukushima University, Division of Human Support System, Faculty of Symbiotic Systems Science, Fukushima (Japan); Ochanomizu University, Leading Graduate School Promotion Center, Tokyo (Japan); Ochanomizu University, Department of Physics, Graduate School of Humanities and Sciences, Tokyo (Japan); Odintsov, Sergei D. [Institut de Ciencies de l' Espai (IEEC-CSIC), Barcelona (Spain); Institucio Catalana de Recerca i Estudis Avancats (ICREA), Barcelona (Spain); Tretyakov, Petr V. [Joined Institute for Nuclear Research, Dubna (Russian Federation)

    2015-07-15

    We explore inflationary cosmology in a theory where there are two scalar fields which non-minimally couple to the Ricci scalar and an additional R{sup 2} term, which breaks the conformal invariance. Particularly, we investigate the slow-roll inflation in the case of one dynamical scalar field and that of two dynamical scalar fields. It is explicitly demonstrated that the spectral index of the scalar mode of the density perturbations and the tensor-to-scalar ratio can be consistent with the observations obtained by the recent Planck satellite. The graceful exit from the inflationary stage is achieved as in convenient R{sup 2} gravity. We also propose the generalization of the model under discussion with three scalar fields. (orig.)

  5. Scalar field with the source in the form of the stress-energy tensor trace as a dark energy model

    CERN Document Server

    Dudko, I G

    2016-01-01

    We consider a scalar-tensor theory of gravitation with the scalar source being the trace of the stress-energy tensor of the scalar field itself and matter. We obtain an example of a numerical solution of the cosmological equations which shows that under some special choice of the scalar parameters, there exists a slow-roll regime in which the modern values of the Hubble and deceleration parameters may be obtained.

  6. On a relation between Liouville field theory and a two component scalar field theory passing through the random walk

    International Nuclear Information System (INIS)

    In this work it is proposed a transformation which is useful in order to simplify non-polynomial potentials given in the form of an exponential. As an application, it is shown that the quantum Liouville field theory may be mapped into a field theory with a polynomial interaction between two scalar fields and a massive vector field

  7. Sterile neutrino dark matter and low scale leptogenesis from a charged scalar

    Energy Technology Data Exchange (ETDEWEB)

    Frigerio, Michele [Laboratoire Charles Coulomb, Montpellier (France); Yaguna, Carlos E. [Universitaet Muenster, Institut fuer Theoretische Physik, Muenster (Germany)

    2015-01-01

    We show that novel paths to dark matter generation and baryogenesis are open when the standard model is extended with three sterile neutrinos N{sub i} and a charged scalar δ{sup +}. Specifically,we propose a new production mechanism for the dark matter particle - multi-keV sterile neutrino, N{sub 1} - that does not depend on the active-sterile mixing angle and does not rely on a large primordial lepton asymmetry. Instead, N{sub 1} is produced, via freeze-in, by the decays of δ{sup +} while it is in equilibrium in the early Universe. In addition, we demonstrate that, thanks to the couplings between the heavier sterile neutrinos N{sub 2,3} and δ{sup +}, baryogenesis via leptogenesis can be realized close to the electroweak scale. The lepton asymmetry is generated either by N{sub 2,3}-decays for masses M{sub 2,3} >or similar TeV, or by N{sub 2,3}-oscillations for M{sub 2,3} ∝ GeV. Experimental signatures of this scenario include an X-ray line from dark matter decays, and the direct production of δ{sup +} at the LHC. This model thus describes a minimal, testable scenario for neutrino masses, the baryon asymmetry, and dark matter. (orig.)

  8. The constraint equations for the Einstein-scalar field system on compact manifolds

    Energy Technology Data Exchange (ETDEWEB)

    Choquet-Bruhat, Yvonne [University of Paris VI, 4 place jussieu, 75005, Paris (France); Isenberg, James [Department of Mathematics, University of Oregon, Eugene, Oregon 97403-5203 (United States); Pollack, Daniel [Department of Mathematics, University of Washington, Box 354350, Seattle, Washington 98195-4350 (United States)

    2007-02-21

    We study the constraint equations for the Einstein-scalar field system on compact manifolds. Using the conformal method we reformulate these equations as a determined system of nonlinear partial differential equations. By introducing a new conformal invariant, which is sensitive to the presence of the initial data for the scalar field, we are able to divide the set of free conformal data into subclasses depending on the possible signs for the coefficients of terms in the resulting Einstein-scalar field Lichnerowicz equation. For many of these subclasses we determine whether or not a solution exists. In contrast to other well studied field theories, there are certain cases, depending on the mean curvature and the potential of the scalar field, for which we are unable to resolve the question of existence of a solution. We consider this system in such generality so as to include the vacuum constraint equations with an arbitrary cosmological constant, the Yamabe equation and even (all cases of) the prescribed scalar curvature problem as special cases.

  9. Reduced Loop Quantization with four Klein-Gordon Scalar Fields as Reference Matter

    CERN Document Server

    Giesel, Kristina

    2016-01-01

    In this paper we perform a reduced phase space quantization of gravity using four Klein-Gordon scalar fields as reference matter as an alternative to the Brown-Kucha\\v{r} dust model in [1] where eight (dust) scalar fields are used. We compare our results to an earlier model by Domagala et. al. [2] where only one Klein-Gordon scalar field was considered as reference matter for the Hamiltonian constraint. As a result we find that the choice of four Klein-Gordon scalar fields as reference matter leads to a reduced dynamical model that cannot be quantized using loop quantum gravity techniques. However, we further discuss a slight generalization of the action for the four Klein-Gordon scalar fields and show that this leads to a model which can be quantized in the framework of loop quantum gravity. Particularly, considering the model by Domagala et. al. [2] and the one introduced in this work we are able to compare Dirac and reduced phase space quantization.

  10. Is Sextans dwarf galaxy in a scalar field dark matter halo?

    CERN Document Server

    Lora, V

    2014-01-01

    The Bose-Einstein condensate/scalar field dark matter model, considers that the dark matter is composed by spinless-ultra-light particles which can be described by a scalar field. This model is an alternative model to the $\\Lambda$-cold dark matter paradigm, and therefore should be studied at galactic and cosmological scales. Dwarf spheroidal galaxies have been very useful when studying any dark matter theory, because the dark matter dominates their dynamics. In this paper we study the Sextans dwarf spheroidal galaxy, embedded in a scalar field dark matter halo. We explore how the dissolution time-scale of the stellar substructures in Sextans, constrain the mass, and the self-interacting parameter of the scalar field dark matter boson. We find that for masses in the range $(0.12< m_{\\phi}<8) \\times10^{-22}$~eV, scalar field dark halos without self-interaction would have cores large enough to explain the longevity of the stellar substructures in Sextans, and small enough mass to be compatible with dynami...

  11. Entanglement Entropy and Variational Methods: Interacting Scalar Fields

    CERN Document Server

    Cotler, Jordan

    2015-01-01

    We develop a variational approximation to the entanglement entropy for scalar $\\phi^4$ theory in 1+1, 2+1, and 3+1 dimensions, and then examine the entanglement entropy as a function of the coupling. We find that in 1+1 and 2+1 dimensions, the entanglement entropy of $\\phi^4$ theory as a function of coupling is monotonically decreasing and convex. While $\\phi^4$ theory with positive bare coupling in 3+1 dimensions is thought to lead to a trivial free theory, we analyze a version of $\\phi^4$ with infinitesimal negative bare coupling, an asymptotically free theory known as precarious $\\phi^4$ theory, and explore the monotonicity and convexity of its entanglement entropy as a function of coupling. Within the variational approximation, the stability of precarious $\\phi^4$ theory is related to the sign of the first and second derivatives of the entanglement entropy with respect to the coupling.

  12. Are black holes a serious threat to scalar field dark matter models?

    CERN Document Server

    Barranco, Juan; Degollado, Juan Carlos; Diez-Tejedor, Alberto; Megevand, Miguel; Alcubierre, Miguel; Núñez, Darío; Sarbach, Olivier

    2011-01-01

    Classical scalar fields have been proposed as possible candidates for the dark matter component of the universe. Given the fact that super-massive black holes seem to exist at the center of most galaxies, in order to be a viable candidate for the dark matter halo a scalar field configuration should be stable in the presence of a central black hole, or at least be able to survive for cosmological time-scales. In the present work we consider a scalar field as a test field on a Schwarzschild background, and study under which conditions one can obtain long-lived configurations. We present a detailed study of the Klein-Gordon equation in the Schwarzschild spacetime, both from an analytical and numerical point of view, and show that indeed there exist quasi-stationary solutions that can remain surrounding a black hole for large time-scales.

  13. Fate of oscillating scalar fields in the thermal bath and their cosmological implications

    CERN Document Server

    Yokoyama, J

    2004-01-01

    Relaxation process of a coherent scalar field oscillation in the thermal bath is investigated using nonequilibrium quantum field theory. The Langevin-type equation of motion is obtained which has a memory term and both additive and multiplicative noise terms. The dissipation rate of the oscillating scalar field is calculated for various interactions such as Yukawa coupling, three-body scalar interaction, and biquadratic interaction. When the background temperature is larger than the oscillation frequency, the dissipation rate arising from the interactions with fermions is suppressed due to the Pauli blocking, while it is enhanced for interactions with bosons due to the induced effect. In both cases, we find that the microphysical detailed balance relation drives the oscillating field to a thermal equilibrium state. That is, for low-momentum modes, the classical fluctuation-dissipation theorem holds and they relax to a state the equipartition law is satisfied, while higher-momentum modes reach the state the nu...

  14. Decoherence and disentanglement of qubits detecting scalar fields in an expanded universe

    CERN Document Server

    Li, Yujie; Shi, Yu

    2016-01-01

    We consider Unruh-Wald qubit detector model adopted for the far future region of an exactly solvable 1+1 dimensional scalar field theory in a Robertson-Walker expanding spacetime. It is shown that the expansion of the universe in its history enhances the decoherence of the qubit coupled with a scalar field. Moreover, we consider two entangled qubits, each locally coupled a scalar field. The expansion of the universe in its history degrades the entanglement between the qubits, and can lead to entanglement sudden death if the initial entanglement is small enough. The details depend on the parameters characterizing the expansion of the universe. This work, albeit on a toy model, suggests that the history of the universe might be probed through the coherent and entanglement behavior of future detectors of quantum fields.

  15. Is the DBI scalar field as fragile as other k -essence fields?

    Science.gov (United States)

    Mukohyama, Shinji; Namba, Ryo; Watanabe, Yota

    2016-07-01

    Caustic singularity formations in shift-symmetric k -essence and Horndeski theories on a fixed Minkowski spacetime were recently argued. In n dimensions, this singularity is the (n -2 )-dimensional plane in spacetime at which second derivatives of a field diverge and the field loses single-valued description for its evolution. This does not necessarily imply a pathological behavior of the system but rather invalidates the effective description. The effective theory would thus have to be replaced by another to describe the evolution thereafter. In this paper, adopting the planar-symmetric 1 +1 -dimensional approach employed in the original analysis, we seek all k -essence theories in which generic simple wave solutions are free from such caustic singularities. Contrary to the previous claim, we find that not only the standard canonical scalar but also the DBI scalar are free from caustics, as far as planar-symmetric simple wave solutions are concerned. Addition of shift-symmetric Horndeski terms does not change the conclusion.

  16. Scalar field reconstruction of power-law entropy-corrected holographic dark energy

    CERN Document Server

    Ebrahimi, Esmaeil

    2010-01-01

    A so called "power-law entropy-corrected holographic dark energy" (PLECHDE) was recently proposed to explain the dark energy dominated universe. This model is based on the power-law corrections to black hole entropy which appear in dealing with the entanglement of quantum fields between inside and outside of the horizon. In this paper, we suggest a correspondence between interacting PLECHDE and tachyon, quintessence, K-essence and dilaton scalar field models of dark energy in a non-flat FRW universe. Then, we reconstruct the potential terms accordingly, and present the dynamical equations which describe the evolution of the scalar field dark energy models.

  17. Anisotropic scalar field emission from TeV scale black hole

    CERN Document Server

    Ida, D; Park, S C; Ida, Daisuke; Oda, Kin-ya; Park, Seong Chan

    2005-01-01

    Black holes are predicted to be copiously produced at the CERN Large Hadron Collider in the scenarios of TeV scale gravity. We report recent progress in studying decay of such a higher dimensional black hole in D=4+n dimensions through the Hawking radiation into brane localized fields taking into account its angular momentum which is indispensable for realistic simulations. Presented is the greybody factors for a scalar field emission, which confirms our previous results in low energy approximation: (i) the existence of super-radiance modes and (ii) the non-trivial angular distribution of radiated scalar field. Phenomenological implications and future plans are discussed.

  18. The innocuousness of adiabatic instabilities in coupled scalar field-dark matter models

    CERN Document Server

    Corasaniti, Pier Stefano

    2010-01-01

    Non-minimally coupled scalar field models suffer of unstable growing modes at the linear perturbation level. The nature of these instabilities depends on the dynamical state of the scalar field. In particular in systems which admit adiabatic solutions, large scale instabilities are suppressed by the slow-roll dynamics of the field. Here we review these results and present a preliminary likelihood data analysis suggesting that along adiabatic solutions coupled models with coupling of order of gravitational strength can provide viable cosmological scenarios satisfying constraints from SN Ia, CMB and large scale structure data.

  19. The dynamical behaviour of homogeneous scalar-field spacetimes with general self-interaction potentials

    CERN Document Server

    Giambó, Roberto; Magli, Giulio

    2008-01-01

    The dynamics of homogeneous Robertson--Walker cosmological models with a self-interacting scalar field source is examined here in full generality, requiring only the scalar field potential to be bounded from below and divergent when the field diverges. In this way we are able to give a unified treatment of all the already studied cases - such as positive potentials which exhibit asymptotically polynomial or exponential behaviors - together with its extension to a much wider set of physically sensible potentials. Since the set includes potentials with negative inferior bound, we are able to give, in particular, the analysis of the asymptotically anti De Sitter states for such cosmologies.

  20. Scalar-tensor gravity with a non-minimally coupled Higgs field and accelerating universe

    Science.gov (United States)

    Sim, Jonghyun; Lee, Tae Hoon

    2016-03-01

    We consider general couplings, including non-minimal derivative coupling, of a Higgs boson field to scalar-tensor gravity and calculate their contributions to the energy density and pressure in Friedmann-Robertson-Walker spacetime. In a special case where the kinetic term of the Higgs field is non-minimally coupled to the Einstein tensor, we seek de Sitter solutions for the cosmic scale factor and discuss the possibility that the late-time acceleration and the inflationary era of our universe can be described by means of scalar fields with self-interactions and the Yukawa potential.

  1. Charged Lepton Flavor Violating Processes and Scalar Leptoquark Decay Branching Ratios in the Colored Zee-Babu Model

    CERN Document Server

    Chang, We-Fu; Wong, Chi-Fong; Xu, Fanrong

    2016-01-01

    We considered a neutrino mass generating model which employs a scalar leptoquark, $\\Delta$, and a scalar diquark, $S$. The new scalars $\\Delta$ and $S$ carry the standard model $SU(3)_c\\times SU(2)_L\\times U(1)_Y$ quantum numbers $(3,1,-1/3)$ and $(6,1,-2/3)$ respectively. The neutrino masses are generated at the two-loop level similar to that in the Zee-Babu model\\cite{Zee-Babu}. And $\\Delta/S$ plays the role of the doubly/singly charged scalar in the Zee-Babu model. With a moderate working assumption that the magnitudes of the six Yukawa couplings between $S$ and the down-type quarks are of the same order, strong connections were found between the neutrino masses and the charged lepton flavor violating(cLFV) processes. In particular, $Z\\rightarrow \\overline{l} l'$, and $l\\rightarrow l' \\gamma$ were studied and it was found that some portions of the parameter space of this model are within the reach of the planned cLFV experiments. Interesting lower bounds on the cLFV processes were predicted that $B(Z\\right...

  2. Stability analysis of 5D gravitational solutions with N bulk scalar fields

    CERN Document Server

    Gherghetta, Tony

    2011-01-01

    We study the stability of 5D gravitational solutions containing an arbitrary number of scalar fields. A closed set of equations is derived which governs the background and perturbations of N scalar fields and the metric, for arbitrary bulk and boundary scalar potentials. In particular the effect of the energy-momentum tensor of the scalar fields on the geometry is fully taken into account, together with all the perturbations of the system. The equations are explicitly written as an eigenvalue problem, which can be readily solved to determine the stability of the system and obtain the properties of the fluctuations, such as masses and couplings. As an example, we study a dynamical soft-wall model with two bulk scalar fields used to model the hadron spectrum of QCD and the Higgs sector of electroweak physics. It is shown that there are no tachyonic modes, and that there is a (radion) mode whose mass is suppressed by a large logarithm compared to that of the other Kaluza-Klein modes.

  3. Linearization stability of coupled gravitational and scalar fields in asymptotically flat space-times

    Energy Technology Data Exchange (ETDEWEB)

    Sarayakar, R.V. (Nagpur Univ. (India). Dept. of Mathematics)

    1982-07-01

    Using the methods of Choquet-Bruhat, Fischer and Marsden and using weighted Sobolev spaces developed recently by Christodoulou and Choquet-Bruhat, it is proved that the Einstein field equations coupled with self-gravitating scalar fields are linearization stable in asymptotically flat space-times.

  4. Complex scalar field in strictly stationary Einstein-Maxwell-axion-dilaton spacetime with negative cosmological constant

    OpenAIRE

    Bakon, Bartlomiej; Rogatko, Marek

    2013-01-01

    We proved that strictly stationary Einstein-Maxwell-axion-dilaton spacetime with negative cosmological constant could not support a nontrivial configuration of complex scalar fields. We considered the general case of the arbitrary number of U(1) gauge fields in the theory under consideration.

  5. Closed star product on noncommutative $\\mathbb{R}^3$ and scalar field dynamics

    CERN Document Server

    Jurić, Tajron; Wallet, Jean-Christophe

    2016-01-01

    We consider the noncommutative space $\\mathbb{R}^3_\\theta$, a deformation of $\\mathbb{R}^3$ for which the star product is closed for the trace functional. We study one-loop IR and UV properties of the 2-point function for real and complex noncommutative scalar field theories with quartic interactions and Laplacian on $\\mathbb{R}^3$ as kinetic operator. We find that the 2-point functions for these noncommutative scalar field theories have no IR singularities in the external momenta, indicating the absence of UV/IR mixing. We also find that the 2-point functions are UV finite with the deformation parameter $\\theta$ playing the role of a natural UV cut-off. The possible origin of the absence of UV/IR mixing in noncommutative scalar field theories on $\\mathbb{R}^3_\\theta$ as well as on $\\mathbb{R}^3_\\lambda $, another deformation of $\\mathbb{R}^3$, is discussed.

  6. Revisiting the spectrum of a scalar field in an anisotropic universe

    CERN Document Server

    Kim, Hyeong-Chan

    2012-01-01

    We revisit the issue on signatures of pre-inflationary background anisotropy by considering the quantization of a massless and minimally coupled scalar field in an axially symmetric Kasner background, mimicking cosmological perturbations. We show that the power spectrum of the scalar field fluctuation has a negligible difference from the standard inflation in the non-planar directions, but it has a sharp peak around the symmetry plane. For the non-planar high-momentum modes, we use the WKB approximation for the first period and the asymptotic approximation based on the de Sitter solution for the next period. At the boundary, two mode functions have the same accuracy with error of $O({H_{i}}/k)$. We calculate the approximation up to the order of $({H_{i}}/k)^6$ and show that the power spectrum of the scalar field fails to get corrections until we execute the approximation up to $6^{\\rm th}$ order.

  7. Adiabatic Ekpyrosis: Scale-Invariant Curvature Perturbations from a Single Scalar Field in a Contracting Universe

    CERN Document Server

    Khoury, Justin

    2009-01-01

    The universe can be made flat and smooth by undergoing a phase of ultra-slow (ekpyrotic) contraction with equation of state w >> 1, a condition that is achievable with a single, canonical scalar field and conventional general relativity. It has been argued, though, that another goal, generating scale-invariant density perturbations, requires at least two scalar fields and a two-step process that first produces entropy fluctuations and then converts them to curvature perturbations. In this paper, we exploit a loophole in the argument and introduce an ekpyrotic model based on a single, canonical scalar field that utilizes a purely "adiabatic mechanism" to generate nearly scale-invariant curvature fluctuations. The curvature perturbation tends to a constant at long wavelengths, indicating that the background evolution is a dynamical attractor. The resulting spectrum is slightly red with distinctive non-gaussian fluctuations.

  8. Holographic dark energy in Brans-Dicke cosmology with chameleon scalar field

    Energy Technology Data Exchange (ETDEWEB)

    Setare, M.R., E-mail: rezakord@ipm.i [Department of Science of Bijar, University of Kurdistan, Bijar (Iran, Islamic Republic of); Jamil, Mubasher, E-mail: mjamil@camp.edu.p [Center for Advanced Mathematics and Physics, National University of Sciences and Technology, Rawalpindi 46000 (Pakistan)

    2010-06-07

    We study a cosmological implication of holographic dark energy in the Brans-Dicke gravity. We employ the holographic model of dark energy to obtain the equation of state for the holographic energy density in non-flat (closed) universe enclosed by the event horizon measured from the sphere of horizon named L. Our analysis shows that one can obtain the phantom crossing scenario if the model parameter {alpha} (of order unity) is tuned accordingly. Moreover, this behavior is achieved by treating the Brans-Dicke scalar field as a Chameleon scalar field and taking a non-minimal coupling of the scalar field with matter. Hence one can generate phantom-like equation of state from a holographic dark energy model in non-flat universe in the Brans-Dicke cosmology framework.

  9. The Local Effects of Cosmological Variations in Physical 'Constants' and Scalar Fields I. Spherically Symmetric Spacetimes

    CERN Document Server

    Shaw, D J; Barrow, John D.; Shaw, Douglas J.

    2006-01-01

    We apply the method of matched asymptotic expansions to analyse whether cosmological variations in physical `constants' and scalar fields are detectable, locally, on the surface of local gravitationally bound systems such as planets and stars, or inside virialised systems like galaxies and clusters. We assume spherical symmetry and derive a sufficient condition for the local time variation of the scalar fields that drive varying constants to track the cosmological one. We calculate under number of specific examples in detail by matching the Schwarzschild spacetime to spherically symmetric inhomogeneous Tolman-Bondi metrics in an intermediate region by rigorously construction matched asymptotic expansions on cosmological and local astronomical scales which overlap in an intermediate domain. We conclude that, independent of the details of the scalar-field theory describing the varying 'constant', the condition for cosmological variations to be measured locally is almost always satisfied in physically realistic ...

  10. Entanglement Entropy Renormalization for the NC scalar field coupled to classical BTZ geometry

    CERN Document Server

    Jurić, Tajron

    2016-01-01

    In this work, we consider a noncommutative (NC) massless scalar field coupled to the classical nonrotational BTZ geometry. In a manner of the theories where the gravity emerges from the underlying scalar field theory, we study the effective action and the entropy derived from this noncommutative model. In particular, the entropy is calculated by making use of the two different approaches, the brick wall method and the heat kernel method designed for spaces with conical singularity. We show that the UV divergent structures of the entropy, obtained through these two different methods, agree with each other. It is also shown that the same renormalization condition that removes the infinities from the effective action can also be used to renormalize the entanglement entropy for the same system. Besides, the interesting feature of the NC model considered here is that it allows an interpretation in terms of an equivalent system comprising of a commutative massive scalar field, but in a modified geometry; that of th...

  11. Bohm Quantum Trajectories of Scalar Field in Trans-Planckian Physics

    Directory of Open Access Journals (Sweden)

    Jung-Jeng Huang

    2012-01-01

    Full Text Available In lattice Schrödinger picture, we investigate the possible effects of trans-Planckian physics on the quantum trajectories of scalar field in de Sitter space within the framework of the pilot-wave theory of de Broglie and Bohm. For the massless minimally coupled scalar field and the Corley-Jacobson type dispersion relation with sextic correction to the standard-squared linear relation, we obtain the time evolution of vacuum state of the scalar field during slow-roll inflation. We find that there exists a transition in the evolution of the quantum trajectory from well before horizon exit to well after horizon exit, which provides a possible mechanism to solve the riddle of the smallness of the cosmological constant.

  12. Bulk scalar field in brane-worlds with induced gravity inspired by the L(R) term

    Energy Technology Data Exchange (ETDEWEB)

    Heydari-Fard, M. [Department of Physics, The University of Qom, Qom 37185-359 (Iran, Islamic Republic of); Sepangi, H.R., E-mail: heydarifard@qom.ac.ir, E-mail: hr-sepangi@sbu.ac.ir [Department of Physics, Shahid Beheshti University, Evin, Tehran 19839 (Iran, Islamic Republic of)

    2009-01-15

    We obtain the effective field equations in a brane-world scenario within the framework of a DGP model where the action on the brane is an arbitrary function of the Ricci scalar, L(R), and the bulk action includes a scalar field in the matter Lagrangian. We obtain the Friedmann equations and acceleration conditions in the presence of the bulk scalar field for the R{sup n} term in four-dimensional gravity.

  13. Is Sextans dwarf galaxy in a scalar field dark matter halo?

    Energy Technology Data Exchange (ETDEWEB)

    Lora, V. [Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg (Germany); Magaña, Juan, E-mail: vlora@ari.uni-heidelberg.de, E-mail: juan.magana@uv.cl [Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Avda. Gran Bretaña 1111, Valparaíso (Chile)

    2014-09-01

    The Bose-Einstein condensate/scalar field dark matter model, considers that the dark matter is composed by spinless-ultra-light particles which can be described by a scalar field. This model is an alternative model to the Λ-cold dark matter paradigm, and therefore should be studied at galactic and cosmological scales. Dwarf spheroidal galaxies have been very useful when studying any dark matter theory, because the dark matter dominates their dynamics. In this paper we study the Sextans dwarf spheroidal galaxy, embedded in a scalar field dark matter halo. We explore how the dissolution time-scale of the stellar substructures in Sextans, constrain the mass, and the self-interacting parameter of the scalar field dark matter boson. We find that for masses in the range (0.12< m{sub φ}<8) ×10{sup -22} eV, scalar field dark halos without self-interaction would have cores large enough to explain the longevity of the stellar substructures in Sextans, and small enough mass to be compatible with dynamical limits. If the self-interacting parameter is distinct to zero, then the mass of the boson could be as high as m{sub φ}≈2×10{sup -21} eV, but it would correspond to an unrealistic low mass for the Sextans dark matter halo . Therefore, the Sextans dwarf galaxy could be embedded in a scalar field/BEC dark matter halo with a preferred self-interacting parameter equal to zero.

  14. Is Sextans dwarf galaxy in a scalar field dark matter halo?

    International Nuclear Information System (INIS)

    The Bose-Einstein condensate/scalar field dark matter model, considers that the dark matter is composed by spinless-ultra-light particles which can be described by a scalar field. This model is an alternative model to the Λ-cold dark matter paradigm, and therefore should be studied at galactic and cosmological scales. Dwarf spheroidal galaxies have been very useful when studying any dark matter theory, because the dark matter dominates their dynamics. In this paper we study the Sextans dwarf spheroidal galaxy, embedded in a scalar field dark matter halo. We explore how the dissolution time-scale of the stellar substructures in Sextans, constrain the mass, and the self-interacting parameter of the scalar field dark matter boson. We find that for masses in the range (0.12< mφ<8) ×10-22 eV, scalar field dark halos without self-interaction would have cores large enough to explain the longevity of the stellar substructures in Sextans, and small enough mass to be compatible with dynamical limits. If the self-interacting parameter is distinct to zero, then the mass of the boson could be as high as mφ≈2×10-21 eV, but it would correspond to an unrealistic low mass for the Sextans dark matter halo . Therefore, the Sextans dwarf galaxy could be embedded in a scalar field/BEC dark matter halo with a preferred self-interacting parameter equal to zero

  15. Interacting Entropy-Corrected Holographic Scalar Field Models in Non-Flat Universe

    International Nuclear Information System (INIS)

    In this work we establish a correspondence between the tachyon, k-essence and dilaton scalar field models with the interacting entropy-corrected holographic dark (ECHD) model in non-flat FRW universe. The reconstruction of potentials and dynamics of these scalar fields according to the evolutionary behavior of the interacting ECHDE model are done. It has been shown that the phantom divide can not be crossed in ECHDE tachyon model while it is achieved for ECHDE k-essence and ECHDE dilaton scenarios. At last we calculate the limiting case of interacting ECHDE model, without entropy-correction. (geophysics, astronomy, and astrophysics)

  16. Quintessential inflation with canonical and noncanonical scalar fields and Planck 2015 results

    CERN Document Server

    Geng, Chao-Qiang; Myrzakulov, R; Sami, M; Saridakis, Emmanuel N

    2015-01-01

    We investigate two classes of models of quintessential inflation, based upon canonical as well as noncanonical scalar fields. In particular, introducing potentials steeper than the standard exponential, we construct models that can give rise to a successful inflationary phase, with signatures consistent with Planck 2015 results. Additionally, using nonminimal coupling of the scalar field with massive neutrino matter, we obtain the standard thermal history of the Universe, with late-time cosmic acceleration as the last stage of evolution. In both cases, inflation and late-time acceleration are connected by a tracker solution.

  17. Confinement and stability in presence of scalar fields and perturbation in the bulk

    CERN Document Server

    Bhattacharya, Pinaki

    2014-01-01

    In this paper we have considered a five-dimensional warped product spacetime with spacelike extra dimension and with a scalar field source in the bulk. We have studied the dynamics of the scalar field under different types of potential in an effort to explain the confinement of particles in the five-dimensional spacetime. The behaviour of the system is determined from the nature of damping force on the system. We have also examined the nature of the effective potential under different circumstances. Lastly we have studied the system to determine whether or not the system attains asymptotically stable condition for both unperturbed and perturbed condition.

  18. New holographic scalar field models of dark energy in non-flat universe

    Energy Technology Data Exchange (ETDEWEB)

    Karami, K., E-mail: KKarami@uok.ac.i [Department of Physics, University of Kurdistan, Pasdaran St., Sanandaj (Iran, Islamic Republic of); Research Institute for Astronomy and Astrophysics of Maragha (RIAAM), Maragha (Iran, Islamic Republic of); Fehri, J. [Department of Physics, University of Kurdistan, Pasdaran St., Sanandaj (Iran, Islamic Republic of)

    2010-02-08

    Motivated by the work of Granda and Oliveros [L.N. Granda, A. Oliveros, Phys. Lett. B 671 (2009) 199], we generalize their work to the non-flat case. We study the correspondence between the quintessence, tachyon, K-essence and dilaton scalar field models with the new holographic dark energy model in the non-flat FRW universe. We reconstruct the potentials and the dynamics for these scalar field models, which describe accelerated expansion of the universe. In the limiting case of a flat universe, i.e. k=0, all results given in [L.N. Granda, A. Oliveros, Phys. Lett. B 671 (2009) 199] are obtained.

  19. Cosmological dynamics of scalar fields with kinetic corrections: Beyond the exponential potential

    CERN Document Server

    Dutta, Jibitesh; Tamanini, Nicola

    2016-01-01

    We expand the dynamical systems investigation of cosmological scalar fields characterised by kinetic corrections presented in [N. Tamanini, Phys. Rev. D 89 (2014) 083521]. In particular we do not restrict the analysis to exponential potentials only, but we consider arbitrary scalar field potentials and derive general results regarding the corresponding cosmological dynamics. Two specific potentials are then used as examples to show how these models can be employed not only to describe dark energy, but also to achieve dynamical crossing of the phantom barrier at late times. Stability and viability issues at the classical level are also discussed.

  20. Scalar-field cosmological and collapse models with general self-interaction potentials

    Energy Technology Data Exchange (ETDEWEB)

    Giambo, Roberto; Giannoni, Fabio [Dipartimento di Matematica e Informatica, Universita di Camerino (Italy); Magli, Giulio, E-mail: roberto.giambo@unicam.i, E-mail: fabio.giannoni@unicam.i, E-mail: magli@mate.polimi.i [Dipartimento di Matematica, Politecnico di Milano (Italy)

    2009-10-01

    We present the results of the investigation of a wide class of self-interacting, self-gravitating homogeneous scalar fields models, characterized by quite general conditions on the scalar field potential, and including both asymptotically polynomial and exponential behaviors. We show that the generic evolution is always divergent in a finite time, and this result is used to construct cosmological models as well as radiating collapsing star models of the Vaidya type - for the latter it turns out that black holes are generically formed.

  1. Possible evolution of a bouncing universe in cosmological models with non-minimally coupled scalar fields

    CERN Document Server

    Pozdeeva, Ekaterina O; Toporensky, Alexey V; Vernov, Sergey Yu

    2016-01-01

    We explore dynamics of cosmological models with bounce solutions evolving on a spatially flat Friedmann-Lemaitre-Robertson-Walker background. We consider cosmological models that contain the Hilbert-Einstein curvature term, the induced gravity term with a negative coupled constant, and even polynomial potentials of the scalar field. Bounce solutions with non-monotonic Hubble parameters have been obtained and analyzed. The case when the scalar field has the conformal coupling and the Higgs potential with an opposite sign is studied in detail. In this model the evolution of the Hubble parameter of the bounce solution essentially depends on the sign of the cosmological constant.

  2. Vanishing Dimensions in Four Dimensional Cosmology with Nonminimal Derivative Coupling of Scalar Field

    CERN Document Server

    Suroso, Agus

    2014-01-01

    We discussed a mechanism that allows the universe to start from lower dimension ($d < 4$) in its very early era and evolves to four dimension at the end of the process. The mechanism is generated by a nonminimal derivative coupling of scalar field, where derivative terms of the scalar field coupled to curvature tensor. We solve the Einstein equations for a limit of large and nearly constant Hubble parameter and analyze the evolution of the Hubble parameter in this limit. The lower-dimensionality in early universe has advantages in the context of unification theory.

  3. Analytical solutions in rotating linear dilaton black holes: Hawking radiation of charged massive scalar particles

    OpenAIRE

    Sakalli, I.

    2016-01-01

    Hawking radiation of charged massive spin-0 particles are studied in the gravitational, electromagnetic, dilaton, and axion fields of rotating linear dilaton black holes. In this geometry, we separate the covariant Klein--Gordon equation into radial and angular parts and obtain the exact solutions of both the equations in terms of the confluent Heun functions. Using the radial solution, we analyze the behavior of the wave solutions near the event horizon of the rotating linear dilaton black h...

  4. A scalar field governed cosmological model from noncompact Kaluza-Klein theory

    CERN Document Server

    Aguilar, J E M; Saenz, F A; Aguilar, Jose Edgar Madriz; Bellini, Mauricio; Saenz, Francisco Astorga

    2004-01-01

    This paper is a review of a recently introduced cosmological model from a noncompact Kaluza-Klein theory for a single scalar field minimally coupled to gravity. We obtain that the 4D scalar potential has a geometrical origin and assume different representations in different frames. It should be responsible for the expansion of the universe. In this framework we explain the (neutral scalar field governed) evolution of the universe from an initially inflationary expansion that has a change of phase towards a decelerated expansion and thereinafter evolves towards the present day observed accelerated (quintessential) expansion. Finally, using the Hamilton-Jacobi formalism, we study extra force and extra mass from this 5D cosmological model.

  5. Propagator of a scalar field on a stationary slowly varying gravitational background

    CERN Document Server

    Kazinski, P O

    2012-01-01

    The propagator of a scalar field on a stationary slowly varying in space gravitational background is derived retaining only the second derivatives of the metric. The corresponding one-loop effective action is constructed. The propagator and the effective action turn out to depend nontrivially on the Killing vector defining the vacuum state and the Hamiltonian of a scalar field. The Hawking particle production is described in the quasiclassical approximation and the quasiclassical formula for the Hawking temperature is derived. The behaviour of the Unruh detector on a curved background is considered and the quasiclassical formula for the Unruh acceleration determining the Unruh temperature is derived. The radiation reaction problem on a curved background is discussed in view of the new approximate expression for the propagator. The correction to the mass squared of a scalar particle on a stationary gravitational background is obtained. This correction is analogous to the quantum correction to the particle mass...

  6. General relativity limit of Horava-Lifshitz gravity with a scalar field in gradient expansion

    CERN Document Server

    Gumrukcuoglu, A Emir; Wang, Anzhong

    2012-01-01

    We present a fully nonlinear study of long wavelength cosmological perturbations within the framework of the projectable Horava-Lifshitz gravity, coupled to a single scalar field. Adopting the gradient expansion technique, we explicitly integrate the dynamical equations up to any order of the expansion, then restrict the integration constants by imposing the momentum constraint. While the gradient expansion relies on the long wavelength approximation, amplitudes of perturbations do not have to be small. When the $\\lambda\\to 1$ limit is taken, the obtained nonlinear solutions exhibit a continuous behavior at any order of the gradient expansion, recovering general relativity in the presence of a scalar field and the "dark matter as an integration constant". This is in sharp contrast to the results in the literature based on the "standard" (and naive) perturbative approach where in the same limit, the perturbative expansion of the action breaks down and the scalar graviton mode appears to be strongly coupled. We...

  7. Radiation Like Scalar Field and Gauge Fields in Cosmology for a theory with Dynamical Time

    CERN Document Server

    Benisty, David

    2016-01-01

    Cosmological solutions with a scalar field behaving as radiation are obtained, in the context of gravitational theory with dynamical time. The solution requires the spacial curvature of the universe k, to be zero, unlike the standard radiation solutions, which do not impose any constraint on the spacial curvature of the universe. This is because only such $ k=0 $ radiation solutions poses a homothetic Killimg vector. This kind of theory can be used to generalize electromagnetism and other gauge theories, in curved space time, and there are no deviations from standard gauge filed equation (like Maxwell equations) in the case there exist a conformal Killing vector. But there could be departures from Maxwell and Yang Mills equations, for more general space times.

  8. Stationary cylindrically symmetric spacetimes with a massless scalar field and a nonpositive cosmological constant

    Science.gov (United States)

    Erices, Cristián; Martínez, Cristián

    2015-08-01

    The general stationary cylindrically symmetric solution of Einstein-massless scalar field system with a nonpositive cosmological constant is presented. It is shown that the general solution is characterized by four integration constants. Two of these essential parameters have a local meaning and characterize the gravitational field strength. The other two have a topological origin, as they define an improper coordinate transformation that provides the stationary solution from the static one. The Petrov scheme is considered to explore the effects of the scalar field on the algebraic classification of the solutions. In general, these spacetimes are of type I. However, the presence of the scalar field allows us to find a nonvacuum type O solution and a wider family of type D spacetimes, in comparison with the vacuum case. The mass and angular momentum of the solution are computed using the Regge-Teitelboim method in the case of a negative cosmological constant. In absence of a cosmological constant, the curvature singularities in the vacuum solutions can be removed by including a phantom scalar field, yielding nontrivial locally homogeneous spacetimes. These spacetimes are of particular interest, as they have all their curvature invariants constant.

  9. The constraint equations for the Einstein-scalar field system on compact manifolds

    CERN Document Server

    Choquet-Bruhat, Y; Pollack, D; Choquet-Bruhat, Yvonne; Isenberg, James; Pollack, Daniel

    2006-01-01

    We study the constraint equations for the Einstein-scalar field system on compact manifolds. Using the conformal method we reformulate these equations as a determined system of nonlinear partial differential equations. By introducing a new conformal invariant, which is sensitive to the presence of the initial data for the scalar field, we are able to divide the set of free conformal data into subclasses depending on the possible signs for the coefficients of terms in the resulting Einstein-scalar field Lichnerowicz equation. For many of these subclasses we determine whether or not a solution exists. In contrast to other well studied field theories, there are certain cases, depending on the mean curvature and the potential of the scalar field, for which we are unable to resolve the question of existence of a solution. We consider this system in such generality so as to include the vacuum constraint equations with an arbitrary cosmological constant, the Yamabe equation and even (all cases of) the prescribed sca...

  10. On the functional renormalization group for the scalar field on curved background with non-minimal interaction

    Energy Technology Data Exchange (ETDEWEB)

    Shapiro, Ilya L. [Universite de Geneve, Departement de Physique Theorique and Center for Astroparticle Physics, Geneva 4 (Switzerland); Universidade Federal de Juiz de Fora, Departamento de Fisica, ICE, Juiz de Fora, MG (Brazil); Tomsk State Pedagogical University, Tomsk (Russian Federation); Tomsk State University, Tomsk (Russian Federation); Morais Teixeira, Poliane de [Universidade Federal de Juiz de Fora, Departamento de Fisica, ICE, Juiz de Fora, MG (Brazil); SISSA, Trieste (Italy); Wipf, Andreas [Friedrich-Schiller-Universitaet, Theoretisch-Physikalisches-Institut, Jena (Germany)

    2015-06-15

    The running of the non-minimal parameter ξ of the interaction of the real scalar field and scalar curvature is explored within the non-perturbative setting of the functional renormalization group (RG). We establish the RG flow in curved space-time in the scalar field sector, in particular derive an equation for the non-minimal parameter. The RG trajectory is numerically explored for different sets of initial data. (orig.)

  11. New models for two real scalar fields and their kinklike solutions

    CERN Document Server

    Alonso-Izquierdo, A; Losano, L; Guilarte, J Mateos

    2013-01-01

    In this work we study the presence of kinks in models described by two real scalar fields in bi-dimensional space-time. We generate new two-field models, constructed from distinct but important one-field models, and we solve them with techniques that we introduce in the current work. We illustrate the results with several examples of current interest to high energy physics.

  12. Contribution to studies of scattering amplitudes and their behaviour at high energies in scalar field theory

    International Nuclear Information System (INIS)

    Scattering amplitudes are studied in scalar field theory. The aim of the work carried out is to obtain valid results for all values of the coupling constant, emphasis being given to high energy behavior. A perturbation approach is first presented, the various integral equations are then written in the framework of the multiperipheral and then Bethe-Salpeter models

  13. Constant mean curvature solutions of the Einstein-scalar field constraint equations on asymptotically hyperbolic manifolds

    Energy Technology Data Exchange (ETDEWEB)

    Sakovich, Anna, E-mail: sakovich@math.kth.s [Institutionen foer Matematik, Kungliga Tekniska Hoegskolan, 100 44 Stockholm (Sweden)

    2010-12-21

    We follow the approach employed by Y Choquet-Bruhat, J Isenberg and D Pollack in the case of closed manifolds and establish existence and non-existence results for constant mean curvature solutions of the Einstein-scalar field constraint equations on asymptotically hyperbolic manifolds.

  14. The Einstein-scalar field constraint equations on asymptotically hyperbolic manifolds

    CERN Document Server

    Sakovich, Anna

    2009-01-01

    We follow the approach employed by Y. Choquet-Bruhat, J. Isenberg and D. Pollack in the case of closed manifolds and establish existence and non-existence results for the Einstein-scalar field constraint equations on asymptotically hyperbolic manifolds.

  15. On cosmological bounces and Lorentzian wormholes in Galileon theories with extra scalar field

    CERN Document Server

    Kolevatov, R

    2016-01-01

    We study whether it is possible to design a "classical" bouncing cosmology or static spherically symmetric Lorentzian wormhole in cubic Galileon theories interacting with an extra scalar field. We show that bouncing models are always plagued with gradient instabilities, while there are always ghosts in wormhole backgrounds.

  16. Localization of scalar fields in the standing wave braneworld with increasing warp factor

    CERN Document Server

    Gogberashvili, Merab; Midodashvili, Levan

    2011-01-01

    We investigate scalar and tensor fields in the brane model solution for the 5D space-time with standing gravitational waves in the bulk, and show that even in the case of increasing warp factor there exist normalizable zero modes localized on the brane.

  17. Localization of scalar and tensor fields in the standing wave braneworld with increasing warp factor

    Energy Technology Data Exchange (ETDEWEB)

    Gogberashvili, Merab, E-mail: gogber@gmail.com [Andronikashvili Institute of Physics, 6 Tamarashvili St., Tbilisi 0177 (Georgia); Javakhishvili State University, 3 Chavchavadze Ave., Tbilisi 0128 (Georgia); Midodashvili, Pavle, E-mail: pmidodashvili@yahoo.com [Ilia State University, 3/5 Kakutsa Cholokashvili Ave., Tbilisi 0162 (Georgia); Midodashvili, Levan, E-mail: levmid@hotmail.com [Gori University, 53 Chavchavadze St., Gori 1400 (Georgia)

    2011-08-19

    We investigate scalar and tensor fields in the brane model solution for the 5D space-time with standing gravitational waves in the bulk and show that even in the case of increasing warp factor there exist normalizable zero modes localized on the brane.

  18. Quasistationary solutions of self-gravitating scalar fields around black holes

    Science.gov (United States)

    Sanchis-Gual, Nicolas; Degollado, Juan Carlos; Montero, Pedro J.; Font, José A.

    2015-02-01

    Recent perturbative studies have shown the existence of long-lived, quasistationary configurations of scalar fields around black holes. In particular, such configurations have been found to survive for cosmological time scales, which is a requirement for viable dark matter halo models in galaxies based on such types of structures. In this paper we perform a series of numerical relativity simulations of dynamical nonrotating black holes surrounded by self-gravitating scalar fields. We solve numerically the coupled system of equations formed by the Einstein and the Klein-Gordon equations under the assumption of spherical symmetry using spherical coordinates. Our results confirm the existence of oscillating, long-lived, self-gravitating scalar field configurations around nonrotating black holes in highly dynamical spacetimes with a rich scalar field environment. Our numerical simulations are long-term stable and allow for the extraction of the resonant frequencies to make a direct comparison with results obtained in the linearized regime. A by-product of our simulations is the existence of a degeneracy in plausible long-lived solutions of Einstein equations that would induce the same motion of test particles, either with or without the existence of quasibound states.

  19. 2+1-dimensional wormhole from a doublet of scalar fields

    OpenAIRE

    Mazharimousavi, S. Habib; Halilsoy, Mustafa

    2015-01-01

    We present a class of exact solutions in the framework of (2+1)-dimensional Einstein gravity coupled minimally to a doublet of scalar fields. Our solution can be interpreted upon the tuning of parameters as an asymptotically flat wormhole as well as a particle model in 2+1 dimensions.

  20. Renormalization of two-loop diagrams in scalar lattice field theory

    CERN Document Server

    Borasoy, B

    2006-01-01

    We present a method to calculate to very high precision the coefficients of the divergences occuring in two-loop diagrams for a massive scalar field on the lattice. The approach is based on coordinate space techniques and extensive use of the precisely known Green's function.

  1. Greens function of a free massive scalar field on the lattice

    CERN Document Server

    Borasoy, B

    2005-01-01

    We propose a method to calculate the Greens function of a free massive scalar field on the lattice numerically to very high precision. For masses m < 2 (in lattice units) the massive Greens function can be expressed recursively in terms of the massless Greens function and just two additional mass-independent constants.

  2. Out-of-Core Compression and Decompression of Large n-Dimensional Scalar Fields

    Energy Technology Data Exchange (ETDEWEB)

    Ibarria, L; Lindstrom, P; Rossignac, J; Szymczak, A

    2003-05-07

    We present a simple method for compressing very large and regularly sampled scalar fields. Our method is particularly attractive when the entire data set does not fit in memory and when the sampling rate is high relative to the feature size of the scalar field in all dimensions. Although we report results for R{sup 3} and R{sup 4} data sets, the proposed approach may be applied to higher dimensions. The method is based on the new Lorenzo predictor, introduced here, which estimates the value of the scalar field at each sample from the values at processed neighbors. The predicted values are exact when the n-dimensional scalar field is an implicit polynomial of degree n-1. Surprisingly, when the residuals (differences between the actual and predicted values) are encoded using arithmetic coding, the proposed method often outperforms wavelet compression in an L{infinity} sense. The proposed approach may be used both for lossy and lossless compression and is well suited for out-of-core compression and decompression, because a trivial implementation, which sweeps through the data set reading it once, requires maintaining only a small buffer in core memory, whose size barely exceeds a single n-1 dimensional slice of the data.

  3. Backreaction of a massless minimally coupled scalar field from inflationary quantum fluctuations

    NARCIS (Netherlands)

    Glavan, D; Prokopec, T.; Prymidis, V.

    2014-01-01

    In this paper we study a massless, minimally coupled scalar field in a Friedmann-Lemaître-Robertson-Walker space-time with periods of different constant deceleration parameter. We assume the Bunch-Davies vacuum during inflation and then use a sudden matching approximation to match it onto a radiatio

  4. Coherent States and Spontaneous Symmetry Breaking in Light Front Scalar Field Theory

    Energy Technology Data Exchange (ETDEWEB)

    Vary, J.P.; /Iowa State U. /LLNL, Livermore /SLAC; Chakrabarti, D.; /Florida U.; Harindranath, A.; /Saha Inst.; Lloyd, R.; /Arkansas State U.; Martinovic, L.; /Bratislava,; Spence, J.R.; /Iowa State U.

    2005-12-14

    Recently developed nuclear many-body techniques provide novel results when applied to constituent quark models and to light-front scalar field theory. We show how spontaneous symmetry breaking arises and is consistent with a coherent state ansatz in a variational treatment. The kink and the kink-antikink topological features are identified and the onset of symmetry restoration is demonstrated.

  5. Non - Topological Solitons in a Non-minimally Coupled Scalar Field Induced Gravity Theory

    CERN Document Server

    Lohiya, Daksh

    2016-01-01

    Properties of soliton stars that could be expected to naturally arise out of a first order phase transition in non-minimally coupled scalar-field-induced gravity theories are investigated. Of particular interest are configurations, similar to Lee-Wick stars, with vanishing effective gravitational constant in the interiors.

  6. Anomalous scaling of a scalar field advected by turbulence

    Energy Technology Data Exchange (ETDEWEB)

    Kraichnan, R.H. [Robert H. Kraichnan, Inc., Santa Fe, NM (United States)

    1995-12-31

    Recent work leading to deduction of anomalous scaling exponents for the inertial range of an advected passive field from the equations of motion is reviewed. Implications for other turbulence problems are discussed.

  7. Scalar Field Dynamics Classical, Quantum and in Between

    CERN Document Server

    Salle, M; Vink, Jeroen C

    2000-01-01

    Using a Hartree ensemble approximation, we investigate the dynamics of the \\phi^4 model in 1+1 dimensions. We find that the fields initially thermalize with a Bose-Einstein distribution for the fields. Gradually, however, the distribution changes towards classical equipartition. Using suitable initial conditions quantum thermalization is achieved much faster than the onset of this undesirable equipartition. We also show how the numerical efficiency of our method can be significantly improved.

  8. Unified dark energy and dark matter from a scalar field different from quintessence

    OpenAIRE

    Gao, Changjun; Kunz, Martin; Liddle, Andrew R.; Parkinson, David

    2009-01-01

    We explore unification of dark matter and dark energy in a theory containing a scalar field of non-Lagrangian type, obtained by direct insertion of a kinetic term into the energy-momentum tensor. This scalar is different from quintessence, having an equation of state between -1 and 0 and a zero sound speed in its rest frame. We solve the equations of motion for an exponential potential via a rewriting as an autonomous system, and demonstrate the observational viability of the scenario, for su...

  9. Lorentz-invariant and Lorentz-non-invariant aspects of a scalar tachyon field Lagrangian and the scalar tachyon Feynman propagator

    CERN Document Server

    Perepelitsa, Vassili F

    2016-01-01

    Some features of a Lorentz-violating (but Lorentz-covariant) Lagrangian of a scalar tachyon field are considered in this note. It is shown that the equation of motion and the Feynman propagator resulting from it are Lorentz-invariant, while the Lorentz symmetry of the suggested tachyon field model can be defined as spontaneously broken.

  10. In-Flight spacecraft magnetic field monitoring using scalar/vector gradiometry

    DEFF Research Database (Denmark)

    Primdahl, Fritz; Risbo, Torben; Merayo, José M.G.;

    2006-01-01

    Earth magnetic field mapping from planetary orbiting satellites requires a spacecraft magnetic field environment control program combined with the deployment of the magnetic sensors on a boom in order to reduce the measurement error caused by the local spacecraft field. Magnetic mapping missions...... the spacecraft centre-of-gravity. In line with the classical dual vector sensors technique for monitoring the spacecraft magnetic field, this paper proposes and demonstrates that a similar combined scalar/vector gradiometry technique is feasible by using the measurements from the boom-mounted scalar and vector...... sensors onboard the Oersted satellite. For Oersted, a large difference between the pre-flight determined spacecraft magnetic field and the in-flight estimate exists causing some concern about the general applicability of the dual sensors technique....

  11. Scalar Field Probes of Power-Law Space-Time Singularities

    CERN Document Server

    Blau, Matthias; Weiss, S; Blau, Matthias; Frank, Denis; Weiss, Sebastian

    2006-01-01

    We analyse the effective potential of the scalar wave equation near generic space-time singularities of power-law type (Szekeres-Iyer metrics) and show that the effective potential exhibits a universal and scale invariant leading x^{-2} inverse square behaviour in the ``tortoise coordinate'' x provided that the metrics satisfy the strict Dominant Energy Condition (DEC). This result parallels that obtained in hep-th/0403252 for probes consisting of families of massless particles (null geodesic deviation, a.k.a. the Penrose Limit). The detailed properties of the scalar wave operator depend sensitively on the numerical coefficient of the x^{-2}-term, and as one application we show that timelike singularities satisfying the DEC are quantum mechanically singular in the sense of the Horowitz-Marolf (essential self-adjointness) criterion. We also comment on some related issues like the near-singularity behaviour of the scalar fields permitted by the Friedrichs extension.

  12. Vacuum stability of a general scalar potential of a few fields

    Energy Technology Data Exchange (ETDEWEB)

    Kannike, Kristjan [NICPB, Tallinn (Estonia)

    2016-06-15

    We calculate analytical vacuum stability or bounded from below conditions for general scalar potentials of a few fields. After a brief review of copositivity, we show how to find positivity conditions for more complicated potentials. We discuss the vacuum stability conditions of the general potential of two real scalars, without and with the Higgs boson included in the potential. As further examples, we give explicit vacuum stability conditions for the two Higgs doublet model with no explicit CP breaking, and for the Z{sub 3} scalar dark matter with an inert doublet and a complex singlet. We give a short overview of positivity conditions for tensors of quartic couplings via tensor eigenvalues. (orig.)

  13. A parametric study on the time scales of the scalar field in turbulent premixed flames

    International Nuclear Information System (INIS)

    An important new development in modeling premixed turbulent combustion is the use of scalar scales which are directly measurable by experiments. An example of such a model relates the mean reaction rates to the temporal or spatial characteristics of instantaneous flame front crossings. These scalar statistics can be obtained by one- point two-time measurements of the scalar field or by two- dimensional laser tomography. The evolution of these scales through the flame brush is central to this modeling framework since the mean creation rate of products may be directly related to them. The cold flow characteristics are determined by Laser Doppler anemometry. The instantaneous flame structure is explored by one-point laser induced Rayleigh scattering technique. Laser tomography is used to determine some spatial statistics of the investigated flames

  14. Entanglement Growth after a Global Quench in Free Scalar Field Theory

    CERN Document Server

    Cotler, Jordan S; Mezei, Márk; Mueller, Mark T

    2016-01-01

    We compute the entanglement and R\\'enyi entropy growth after a global quench in various dimensions in free scalar field theory. We study two types of quenches: a boundary state quench and a global mass quench. Both of these quenches are investigated for a strip geometry in 1, 2, and 3 spatial dimensions, and for a spherical geometry in 2 and 3 spatial dimensions. We compare the numerical results for massless free scalars in these geometries with the predictions of the analytical quasiparticle model based on EPR pairs, and find excellent agreement in the limit of large region sizes. At subleading order in the region size, we observe an anomalous logarithmic growth of entanglement coming from the zero mode of the scalar.

  15. Divergence of Electric Field of Continuous and of a Point Charge for Relativistic and non-Relativistic Motion

    CERN Document Server

    Zhakatayev, Altay

    2016-01-01

    In this paper we considered divergence of electric and of magnetic fields for four cases: classical point charge, classical continuous charge, relativistic point and relativistic continuous charges. Results for classical and relativistic point charges are the same as in literature, i.e. Gauss's law is valid. However results for time-varying classical and relativistic distributed charges indicate that divergence of electric field is not zero even for volumes of space where no charges are present. For these cases original Gauss's law might require modification. Divergence of electric field seems to be far-field type scalar anisotropic field, which is generated by time-varying electric charges or currents. Results indicate that for these effects to be sufficiently large to be experimentally observable the time variation of electric charges and/or of currents should be very fast. Divergence of magnetic field is zero for all cases.

  16. PDF approach for turbulent scalar field: Some recent developments

    Science.gov (United States)

    Gao, Feng

    1993-01-01

    The probability density function (PDF) method has been proven a very useful approach in turbulence research. It has been particularly effective in simulating turbulent reacting flows and in studying some detailed statistical properties generated by a turbulent field There are, however, some important questions that have yet to be answered in PDF studies. Our efforts in the past year have been focused on two areas. First, a simple mixing model suitable for Monte Carlo simulations has been developed based on the mapping closure. Secondly, the mechanism of turbulent transport has been analyzed in order to understand the recently observed abnormal PDF's of turbulent temperature fields generated by linear heat sources.

  17. Power-law modulation of the scalar power spectrum from a heavy field with a monomial potential

    CERN Document Server

    Huang, Qing-Guo

    2016-01-01

    The effects of heavy fields modulate the scalar power spectrum during inflation. We analytically calculate the modulations of the scalar power spectrum from a heavy field with a separable monomial potential, i.e. V(\\phi)~\\phi^n. In general the modulation is characterized by a power-law oscillation which is reduced to the logarithmic oscillation in the case of n=2.

  18. Interacting new agegraphic tachyon, K-essence and dilaton scalar field models of dark energy in non-flat universe

    Energy Technology Data Exchange (ETDEWEB)

    Karami, K., E-mail: KKarami@uok.ac.i [Department of Physics, University of Kurdistan, Pasdaran St., Sanandaj (Iran, Islamic Republic of); Research Institute for Astronomy and Astrophysics of Maragha (RIAAM), Maragha (Iran, Islamic Republic of); Khaledian, M.S.; Felegary, F.; Azarmi, Z. [Department of Physics, University of Kurdistan, Pasdaran St., Sanandaj (Iran, Islamic Republic of)

    2010-03-29

    We study the correspondence between the tachyon, K-essence and dilaton scalar field models with the interacting new agegraphic dark energy model in the non-flat FRW universe. We reconstruct the potentials and the dynamics for these scalar field models, which describe accelerated expansion of the universe.

  19. The charged inflaton and its gauge fields: preheating and initial conditions for reheating

    CERN Document Server

    Lozanov, Kaloian D

    2016-01-01

    We calculate particle production during inflation and in the early stages of reheating after inflation in models with a charged scalar field coupled to Abelian and non-Abelian gauge fields. A detailed analysis of the power spectra of primordial electric fields, magnetic fields and charge fluctuations at the end of inflation and preheating is provided. We carefully account for the Gauss constraints during inflation and preheating, and clarify the role of the longitudinal components of the electric field. We calculate the timescale for the back-reaction of the produced gauge fields on the inflaton condensate, marking the onset of non-linear evolution of the fields. We provide a prescription for initial conditions for lattice simulations necessary to capture the subsequent nonlinear dynamics. On the observational side, we find that the primordial magnetic fields generated are too small to explain the origin of magnetic fields on galactic scales and the charge fluctuations are well within observational bounds for...

  20. Matter fields in the lagrangian loop representation scalar QED

    CERN Document Server

    Aroca, J M; Fort, H; Siri, R

    1995-01-01

    We present the extension of the Lagrangian loop gauge invariant representation in such a way to include matter fields. The partition function of lattice compact U(1)-Higgs model is expressed as a sum over closed as much as open surfaces. We have simulated numerically the loop action equivalent to the Villain form of the action and mapped out the beta-gamma phase diagram of this model.

  1. The average action for scalar fields near phase transitions

    International Nuclear Information System (INIS)

    We compute the average action for fields in two, three and four dimensions, including the effects of wave function renormalization. A study of the one loop evolution equations for the scale dependence of the average action gives a unified picture of the qualitatively different behaviour in various dimensions for discrete as well as abelian and nonabelian continuous symmetry. The different phases and the phase transitions can be infered from the evolution equation. (orig.)

  2. Hamiltonian description of the parametrized scalar field in bounded spatial regions

    CERN Document Server

    G., J Fernando Barbero; Villaseñor, Eduardo J S

    2015-01-01

    We study the Hamiltonian formulation for a parametrized scalar field in a regular bounded spatial region subject to Dirichlet, Neumann and Robin boundary conditions. We generalize the work carried out by a number of authors on parametrized field systems to the interesting case where spatial boundaries are present. The configuration space of our models contains both smooth scalar fields defined on the spatial manifold and spacelike embeddings from the spatial manifold to a target spacetime endowed with a fixed Lorentzian background metric. We pay particular attention to the geometry of the infinite dimensional manifold of embeddings and the description of the relevant geometric objects: the symplectic form on the primary constraint submanifold and the Hamiltonian vector fields defined on it.

  3. Hamiltonian description of the parametrized scalar field in bounded spatial regions

    Science.gov (United States)

    Barbero G, J. Fernando; Margalef-Bentabol, Juan; Villaseñor, Eduardo J. S.

    2016-05-01

    We study the Hamiltonian formulation for a parametrized scalar field in a regular bounded spatial region subject to Dirichlet, Neumann and Robin boundary conditions. We generalize the work carried out by a number of authors on parametrized field systems to the interesting case where spatial boundaries are present. The configuration space of our models contains both smooth scalar fields defined on the spatial manifold and spacelike embeddings from the spatial manifold to a target spacetime endowed with a fixed Lorentzian background metric. We pay particular attention to the geometry of the infinite dimensional manifold of embeddings and the description of the relevant geometric objects: the symplectic form on the primary constraint submanifold and the Hamiltonian vector fields defined on it.

  4. Evolution of scalar fields surrounding black holes on compactified constant mean curvature hypersurfaces

    CERN Document Server

    Morales, Manuel D

    2016-01-01

    Motivated by the goal for high accuracy modeling of gravitational radiation emitted by isolated systems, recently, there has been renewed interest in the numerical solution of the hyperboloidal initial value problem for Einstein's field equations in which the outer boundary of the numerical grid is placed at null infinity. In this article, we numerically implement the tetrad-based approach presented in [J.M. Bardeen, O. Sarbach, and L.T. Buchman, Phys. Rev. D 83, 104045 (2011)] for a spherically symmetric, minimally coupled, self-gravitating scalar field. When this field is massless, the evolution system reduces to a regular, first-order symmetric hyperbolic system of equations for the conformally rescaled scalar field which is coupled to a set of singular elliptic constraints for the metric coefficients. We show how to solve this system based on a numerical finite-difference approximation, obtaining stable numerical evolutions for initial black hole configurations which are surrounded by a spherical shell of...

  5. Efficient, Decentralized Detection of Qualitative Spatial Events in a Dynamic Scalar Field

    OpenAIRE

    Myeong-Hun Jeong; Matt Duckham

    2015-01-01

    This paper describes an efficient, decentralized algorithm to monitor qualitative spatial events in a dynamic scalar field. The events of interest involve changes to the critical points (i.e., peak, pits and passes) and edges of the surface network derived from the field. Four fundamental types of event (appearance, disappearance, movement and switch) are defined. Our algorithm is designed to rely purely on qualitative information about the neighborhoods of nodes in the sensor network and doe...

  6. Magnetic Pressure as a Scalar Representation of Field Effects in Magnetic Suspensions

    OpenAIRE

    Zborowski, Maciej; Moore, Lee R.; Williams, P. Stephen; Chalmers, Jeffrey J.

    2010-01-01

    Magnetic microsphere suspensions undergo complex motion when exposed to finite sources of the magnetic field, such as small permanent magnets. The computational complexity is compounded by a difficulty in choosing a suitable choice of visualization tools because this often requires using the magnetic force vector field in three dimensions. Here we present a potentially simpler approach by using the magnetic pressure. It is a scalar quantity, pm = B2/2μ0, and its usefulness has been already de...

  7. VOFI - A library to initialize the volume fraction scalar field

    Science.gov (United States)

    Bnà, S.; Manservisi, S.; Scardovelli, R.; Yecko, P.; Zaleski, S.

    2016-03-01

    The VOFI library has been developed to accurately calculate the volume fraction field demarcated by implicitly-defined fluid interfaces in Cartesian grids with cubic cells. The method enlists a number of algorithms to compute the integration limits and the local height function, that is the integrand of a double Gauss-Legendre integration with a variable number of nodes. Tests in two and three dimensions are presented to demonstrate the accuracy of the method and are provided in the software distribution with C/C++ and FORTRAN interfaces.

  8. Vacuum energy density and pressure of a massive scalar field

    OpenAIRE

    Mera, Fernando Daniel; Fulling, S. A.

    2014-01-01

    With a view toward application of the Pauli-Villars regularization method to the Casimir energy of boundaries, we calculate the expectation values of the components of the stress tensor of a confined massive field in 1+1 space-time dimensions. Previous papers by Hays and Fulling are bridged and generalized. The Green function for the time-independent Schrodinger equation is constructed from the Green function for the whole line by the method of images; equivalently, the one-dimensional system...

  9. Vacuum energy density and pressure of a massive scalar field

    Science.gov (United States)

    Mera, Fernando Daniel; Fulling, S. A.

    2015-06-01

    With a view toward application of the Pauli-Villars regularization method to the Casimir energy of boundaries, we calculate the expectation values of the components of the stress tensor of a confined massive field in 1+1 space-time dimensions. Previous papers by Hays and Fulling are bridged and generalized. The Green function for the time-independent Schrödinger equation is constructed from the Green function for the whole line by the method of images; equivalently, the one-dimensional system is solved exactly in terms of closed classical paths and periodic orbits. Terms in the energy density and in the eigenvalue density attributable to the two boundaries individually and those attributable to the confinement of the field to a finite interval are distinguished so that their physical origins are clear. Then the pressure is found similarly from the cylinder kernel, the Green function associated most directly with an exponential frequency cutoff of the Fourier mode expansion. Finally, we discuss how the theory could be rendered finite by the Pauli-Villars method.

  10. Vacuum energy density and pressure of a massive scalar field

    CERN Document Server

    Mera, Fernando Daniel

    2014-01-01

    With a view toward application of the Pauli-Villars regularization method to the Casimir energy of boundaries, we calculate the expectation values of the components of the stress tensor of a confined massive field in 1+1 space-time dimensions. Previous papers by Hays and Fulling are bridged and generalized. The Green function for the time-independent Schrodinger equation is constructed from the Green function for the whole line by the method of images; equivalently, the one-dimensional system is solved exactly in terms of closed classical paths and periodic orbits. Terms in the energy density and in the eigenvalue density attributable to the two boundaries individually and those attributable to the confinement of the field to a finite interval are distinguished so that their physical origins are clear. Then the pressure is found similarly from the cylinder kernel, the Green function associated most directly with an exponential frequency cutoff of the Fourier mode expansion. Finally, we discuss how the theory ...

  11. On the scalar particle creation by electromagnetic fields in Robertson–Walker spacetime

    Directory of Open Access Journals (Sweden)

    Kenan Sogut

    2015-12-01

    Full Text Available In the present paper, we obtained the scalar particle creation number density by using the Klein–Gordon equation coupled to the electromagnetic fields in the Robertson–Walker spacetime with the help of the Bogoliubov transformation method. We analyzed the resulting expression for the effect of a time-dependent electric field and a constant magnetic field on the particle production rate and found that the strong time-dependent electric field amplifies the particle creation and the magnetic field reduces the rate, in accordance with the previous findings.

  12. Scalar field reconstruction of power-law entropy-corrected holographic dark energy

    International Nuclear Information System (INIS)

    A so-called 'power-law entropy-corrected holographic dark energy' (PLECHDE) was recently proposed to explain the dark energy (DE)-dominated universe. This model is based on the power-law corrections to black hole entropy that appear when dealing with the entanglement of quantum fields between the inside and the outside of the horizon. In this paper, we suggest a correspondence between the interacting PLECHDE and the tachyon, quintessence, K-essence and dilaton scalar field models of DE in a non-flat Friedmann-Robertson-Walker universe. Then, we reconstruct the potential terms accordingly, and present the dynamical equations that describe the evolution of the scalar field DE models.

  13. Scalar field reconstruction of power-law entropy-corrected holographic dark energy

    Energy Technology Data Exchange (ETDEWEB)

    Ebrahimi, Esmaeil [Department of Physics, Shahid Bahonar University, PO Box 76175, Kerman (Iran, Islamic Republic of); Sheykhi, Ahmad, E-mail: eebrahimi@uk.ac.ir, E-mail: sheykhi@uk.ac.ir [Department of Physics, Kerman Branch, Islamic Azad University, Kerman (Iran, Islamic Republic of)

    2011-10-15

    A so-called 'power-law entropy-corrected holographic dark energy' (PLECHDE) was recently proposed to explain the dark energy (DE)-dominated universe. This model is based on the power-law corrections to black hole entropy that appear when dealing with the entanglement of quantum fields between the inside and the outside of the horizon. In this paper, we suggest a correspondence between the interacting PLECHDE and the tachyon, quintessence, K-essence and dilaton scalar field models of DE in a non-flat Friedmann-Robertson-Walker universe. Then, we reconstruct the potential terms accordingly, and present the dynamical equations that describe the evolution of the scalar field DE models.

  14. Scalar field reconstruction of power-law entropy-corrected holographic dark energy

    Science.gov (United States)

    Ebrahimi, Esmaeil; Sheykhi, Ahmad

    2011-10-01

    A so-called 'power-law entropy-corrected holographic dark energy' (PLECHDE) was recently proposed to explain the dark energy (DE)-dominated universe. This model is based on the power-law corrections to black hole entropy that appear when dealing with the entanglement of quantum fields between the inside and the outside of the horizon. In this paper, we suggest a correspondence between the interacting PLECHDE and the tachyon, quintessence, K-essence and dilaton scalar field models of DE in a non-flat Friedmann-Robertson-Walker universe. Then, we reconstruct the potential terms accordingly, and present the dynamical equations that describe the evolution of the scalar field DE models.

  15. Global dynamics and asymptotics for monomial scalar field potentials and perfect fluids

    CERN Document Server

    Alho, Artur; Uggla, Claes

    2015-01-01

    We consider a minimally coupled scalar field with a monomial potential and a perfect fluid in flat FLRW cosmology. We apply local and global dynamical systems techniques to a new three-dimensional dynamical systems reformulation of the field equations on a compact state space. This leads to a visual global description of the solution space and asymptotic behavior. At late times we employ averaging techniques to prove statements about how the relationship between the equation of state of the fluid and the monomial exponent of the scalar field affects asymptotic source dominance and asymptotic manifest self-similarity breaking. We also situate the `attractor' solution in the three-dimensional state space and show that it corresponds to the one-dimensional unstable center manifold of a de Sitter fixed point, located on an unphysical boundary associated with the dynamics at early times. By deriving a center manifold expansion we obtain approximate expressions for the attractor solution. We subsequently improve th...

  16. Asymptotic Tails of Massive Scalar Fields in a Stationary Axisymmetric EMDA Black Hole Geometry

    Institute of Scientific and Technical Information of China (English)

    PAN Qi-Yuan; JING Ji-Liang

    2004-01-01

    The late-time tail behaviour of massive scalar fields is studied analytically in a stationary axisymmetric EinsteinMaxwell Dilaton-Axion (EMDA) black hole geometry. It is shown that the asymptotic behaviour of massive perturbations is dominated by the oscillatory inverse power-law decaying tail t-(l+3/2) sin(μt) at the intermediate late times, and by the asymptotic tail t-5/6 sin(μt) at asymptotically late times, with μ being field mass. Our result seems to suggest that the intermediate tails t-(l+3/2) sin(μt) and the asymptotically tails t-5/6 sin(μt) may be a quite general feature for evolution of massive scalar fields in any four-dimensional asymptotically flat rotating black hole backgrounds.

  17. The Modification of the Scalar Field in dense Nuclear Matter

    Science.gov (United States)

    Rożynek, J.

    2011-04-01

    We show the possible evolution of the nuclear deep inelastic structure function with nuclear density ρ. The nucleon deep inelastic structure function represents distribution of quarks as function of Björken variable x which measures the longitudinal fraction of momentum carried by them during the Deep Inelastic Scattering (DIS) of electrons on nuclear targets. Starting with small density and negative pressure in Nuclear Matter (NM) we have relatively large inter-nucleon distances and increasing role of nuclear interaction mediated by virtual mesons.When the density approaches the saturation point, ρ = ρ0, we have no longer separate mesons and nucleons but eventually modified nucleon Structure Function (SF) in medium. The ratio of nuclear to nucleon SF measured at saturation point is well known as "EMC effect". For larger density, ρ > ρ0, when the localization of quarks is smaller then 0.3 fm, the nucleons overlap. We argue that nucleon mass should start to decrease in order to satisfy the Momentum Sum Rule (MSR) of DIS. These modifications of the nucleon Structure Function (SF) are calculated in the frame of the nuclear Relativistic Mean Field (RMF) convolution model. The correction to the Fermi energy from term proportional to the pressure is very important and its inclusion modifies the Equation of State (EoS) for nuclear matter.

  18. The Modification of the Scalar Field in dense Nuclear Matter

    Directory of Open Access Journals (Sweden)

    Rożynek J.

    2011-04-01

    Full Text Available We show the possible evolution of the nuclear deep inelastic structure function with nuclear density ρ. The nucleon deep inelastic structure function represents distribution of quarks as function of Björken variable x which measures the longitudinal fraction of momentum carried by them during the Deep Inelastic Scattering (DIS of electrons on nuclear targets. Starting with small density and negative pressure in Nuclear Matter (NM we have relatively large inter-nucleon distances and increasing role of nuclear interaction mediated by virtual mesons.When the density approaches the saturation point, ρ = ρ0, we have no longer separate mesons and nucleons but eventually modified nucleon Structure Function (SF in medium. The ratio of nuclear to nucleon SF measured at saturation point is well known as “EMC effect”. For larger density, ρ > ρ0, when the localization of quarks is smaller then 0.3 fm, the nucleons overlap. We argue that nucleon mass should start to decrease in order to satisfy the Momentum Sum Rule (MSR of DIS. These modifications of the nucleon Structure Function (SF are calculated in the frame of the nuclear Relativistic Mean Field (RMF convolution model. The correction to the Fermi energy from term proportional to the pressure is very important and its inclusion modifies the Equation of State (EoS for nuclear matter.

  19. Numerical Models of Cosmological Evolution of the Degenerated Fermi-system of Scalar Charged Particles

    CERN Document Server

    Ignatyev, Yu G

    2014-01-01

    Based on mathematical model of the statistical Fermi system with the interparticle interaction which was constructed in the previous articles, this work offers the construction and analysis of the numerical models of cosmological evolution of the single-component degenerated Fermi system of the scalar particles. The applied mathematics package Mathematica 9 is used for the numerical model construction.

  20. Non-Maximal Tripartite Entanglement Degradation of Dirac and Scalar Fields in Non-Inertial Frames

    Science.gov (United States)

    Salman, Khan; Niaz, Ali Khan; M. K., Khan

    2014-03-01

    The π-tangle is used to study the behavior of entanglement of a nonmaximal tripartite state of both Dirac and scalar fields in accelerated frame. For Dirac fields, the degree of degradation with acceleration of both one-tangle of accelerated observer and π-tangle, for the same initial entanglement, is different by just interchanging the values of probability amplitudes. A fraction of both one-tangles and the π-tangle always survives for any choice of acceleration and the degree of initial entanglement. For scalar field, the one-tangle of accelerated observer depends on the choice of values of probability amplitudes and it vanishes in the range of infinite acceleration, whereas for π-tangle this is not always true. The dependence of π-tangle on probability amplitudes varies with acceleration. In the lower range of acceleration, its behavior changes by switching between the values of probability amplitudes and for larger values of acceleration this dependence on probability amplitudes vanishes. Interestingly, unlike bipartite entanglement, the degradation of π-tangle against acceleration in the case of scalar fields is slower than for Dirac fields.

  1. Scalar and Vector Field Constraints, Deflection of Light and Lensing in Modified Gravity (MOG)

    CERN Document Server

    Moffat, J W

    2014-01-01

    A conformal coupling of the metric in the Jordan frame to the energy-momentum tensor, screens the scalar field gravitational coupling strength $G$ in modified gravity (MOG). The scalar field acquires a mass which depends on the local matter density: the scalar field particle is massive for the Sun and earth, where the density is high compared to low density environments in cosmology and astrophysics. Together with the screening of the vector field $\\phi_\\mu$, this guarantees that solar system tests of gravity are satisfied. The conformal metric is coupled to the electromagnetic matter field and energy-momentum tensor, screening $G$ for the Sun and the deflection of light by the Sun and the Shapiro time delay in MOG are in agreement with general relativity. For galaxies and galactic clusters the enhanced gravitational coupling constant $G$ leads to agreement with gravitational lensing without dark matter. For compact binary pulsars the screening of $G$ removes the monopole and dipole gravitational radiation mo...

  2. On the theory of a non-linear neutral scalar field with spontaneously broken symmetry

    CERN Document Server

    Poluektov, Yu M

    2015-01-01

    On the example of a real scalar field, an approach to quantization of non-linear fields and construction of the perturbation theory with account of spontaneous symmetry breaking is proposed. The method is based on using as the main approximation of the relativistic self-consistent field model, in which the influence of vacuum fluctuations is taken into account in constructing the one-particle states. The solutions of the self-consistent equations determine possible states, which also include the states with broken symmetries. Different states of the field are matched to particles, whose masses are determined by both parameters of the Lagrangian and vacuum fluctuations.

  3. First scalar magnetic anomaly map from CHAMP satellite data indicates weak lithospheric field

    DEFF Research Database (Denmark)

    Maus, S.; Rother, M.; Holme, R.;

    2002-01-01

    and external field model, we remove remaining unmodeled large-scale external contributions from 120 track segments by subtracting a best-fitting uniform field. In order to preserve N/S trending features, the data are not filtered along-track. Direct integration of the spherically gridded data yields......Satellite magnetic anomaly maps derived by different techniques from Magsat/POGO data vary by more than a factor of 2 in the deduced strength of the lithospheric magnetic field. Here, we present a first anomaly map from new CHAMP scalar magnetic field data. After subtracting a recent Ørsted main...

  4. Efficient visualization of unsteady and huge scalar and vector fields

    Science.gov (United States)

    Vetter, Michael; Olbrich, Stephan

    2016-04-01

    and methods, we are developing a stand-alone post-processor, adding further data structures and mapping algorithms, and cooperating with the ICON developers and users. With the implementation of a DSVR-based post-processor, a milestone was achieved. By using the DSVR post-processor the mentioned 3 processes are completely separated: the data set is processed in a batch mode - e.g. on the same supercomputer, which the data is generated on - and the interactive 3D rendering is done afterwards on the scientist's local system. At the actual status of implementation the DSVR post-processor supports the generation of isosurfaces and colored slicers on volume data set time series based on rectilinear grids as well as the visualization of pathlines on time varying flow fields based on either rectilinear grids or prism grids. The software implementation and evaluation is done on the supercomputers at DKRZ, including scalability tests using ICON output files in NetCDF format. The next milestones will be (a) the in-situ integration of the DSVR library in the ICON model and (b) the implementation of an isosurface algorithm for prism grids.

  5. Distributed Sensor Fusion for Scalar Field Mapping Using Mobile Sensor Networks.

    Science.gov (United States)

    La, Hung Manh; Sheng, Weihua

    2013-04-01

    In this paper, autonomous mobile sensor networks are deployed to measure a scalar field and build its map. We develop a novel method for multiple mobile sensor nodes to build this map using noisy sensor measurements. Our method consists of two parts. First, we develop a distributed sensor fusion algorithm by integrating two different distributed consensus filters to achieve cooperative sensing among sensor nodes. This fusion algorithm has two phases. In the first phase, the weighted average consensus filter is developed, which allows each sensor node to find an estimate of the value of the scalar field at each time step. In the second phase, the average consensus filter is used to allow each sensor node to find a confidence of the estimate at each time step. The final estimate of the value of the scalar field is iteratively updated during the movement of the mobile sensors via weighted average. Second, we develop the distributed flocking-control algorithm to drive the mobile sensors to form a network and track the virtual leader moving along the field when only a small subset of the mobile sensors know the information of the leader. Experimental results are provided to demonstrate our proposed algorithms.

  6. Cosmology of an asymptotically free scalar field with spontaneous symmetry breaking

    CERN Document Server

    Huang, Kerson; Tung, Roh-Suan

    2010-01-01

    We solve Einstein's equation with Robertson-Walker metric as an initial-value problem, using as the source of gravity a Halpern-Huang real scalar field, which was derived from renormalization-group analysis, with a potential that exhibits asymptotic freedom and spontaneous symmetry breaking. Both properties are crucial to the formulation of the problem. Numerical solutions show that the universe expands at an accelerated rate, with the radius increasing like the exponential of a power of the time. This is relevant to "dark energy" and "cosmic inflation". Extension to the complex scalar field will make the universe a superfluid. The vortex dynamics that emerges offers explanations for other cosmological problems, namely, matter creation, galactic voids, and the "dark mass".

  7. Vacuum Expectation Value Profiles of the Bulk Scalar Field in the Generalized Randall-Sundrum Model

    CERN Document Server

    Tofighi, A; Farokhtabar, A

    2015-01-01

    In the generalized Randall-Sundrum warped brane-world model the cosmological constant induced on the visible brane can be positive or negative. In this paper we investigate profiles of vacuum expectation value of the bulk scalar field under general Dirichlet andNeumann boundary conditions in the generalized warped brane-worldmodel.We showthat the VEVprofiles generally depend on the value of the brane cosmological constant. We find that the VEV profiles of the bulk scalar field for a visible brane with negative cosmological constant and positive tension are quite distinct fromthose of Randall-Sundrum model. In addition we show that the VEV profiles for a visible brane with large positive cosmological constant are also different from those of the Randall- Sundrum model.We also verify that Goldberger andWise mechanism can work under nonzero Dirichlet boundary conditions in the generalized Randall-Sundrum model.

  8. Nonperturbative dynamics of scalar field theories through the Feynman-Schwinger representation

    Energy Technology Data Exchange (ETDEWEB)

    Cetin Savkli; Franz Gross; John Tjon

    2004-04-01

    In this paper we present a summary of results obtained for scalar field theories using the Feynman-Schwinger (FSR) approach. Specifically, scalar QED and {chi}{sup 2}{phi} theories are considered. The motivation behind the applications discussed in this paper is to use the FSR method as a rigorous tool for testing the quality of commonly used approximations in field theory. Exact calculations in a quenched theory are presented for one-, two-, and three-body bound states. Results obtained indicate that some of the commonly used approximations, such as Bethe-Salpeter ladder summation for bound states and the rainbow summation for one body problems, produce significantly different results from those obtained from the FSR approach. We find that more accurate results can be obtained using other, simpler, approximation schemes.

  9. QCD phase transition with a power law chameleon scalar field in the bulk

    CERN Document Server

    Golanbari, T; Saaidi, Kh

    2014-01-01

    In this work, a brane world model with a perfect fluid on brane and a scalar field on bulk has been used to study quark-hadron phase transition. The bulk scalar field has an interaction with brane matter. This interaction comes into non-conservation relation which describe an energy transfer between bulk and brane. Since quark-hadron transition curly depends on the form of evolution equations therefore modification of energy conservation equation and Friedmann equation comes into some interesting results about the time of transition. The evolution of physical quantities relevant to quantitative of early times namely energy density $\\rho$ temperature $T$ and scale factor $a$ have been considered utilizing two formalisms as crossover formalism and first order phase transition formalism. The results show that the quark-hadron phase transition in occurred about nanosecond after big bang and the general behavior temperature is similar in both of two formalism.

  10. QCD phase transition with a power law chameleon scalar field in the bulk

    Science.gov (United States)

    Golanbari, Tayeb; Mohammadi, Abolhassan; Saaidi, Khaled

    2014-03-01

    In this paper, a braneworld model with a perfect fluid on brane and a scalar field on bulk has been used to study quark-hadron phase transition. The bulk scalar field has an interaction with brane matter. This interaction comes into nonconservation relation which describes an energy transfer between bulk and brane. Since quark-hadron transition truly depends on the form of evolution equations, modification of energy conservation equation and Friedmann equation gives rise to some interesting results about the time of transition. The evolution of physical quantities relevant to the quantitative of early times namely energy density ρ, temperature T and scale factor a have been considered utilizing two formalism, crossover formalism and first-order phase transition formalism. The results show that the quark-hadron phase transition occurred about a nanosecond after big bang and the general behavior temperature is similar in both of two formalism.

  11. Generalized second law of thermodynamics for non-canonical scalar field model with corrected-entropy

    Energy Technology Data Exchange (ETDEWEB)

    Das, Sudipta; Mamon, Abdulla Al [Visva-Bharati, Department of Physics, Santiniketan (India); Debnath, Ujjal [Indian Institute of Engineering Science and Technology, Department of Mathematics, Shibpur, Howrah (India)

    2015-10-15

    In this work, we have considered a non-canonical scalar field dark energy model in the framework of flat FRW background. It has also been assumed that the dark matter sector interacts with the non-canonical dark energy sector through some interaction term. Using the solutions for this interacting non-canonical scalar field dark energy model, we have investigated the validity of generalized second law (GSL) of thermodynamics in various scenarios using first law and area law of thermodynamics. For this purpose, we have assumed two types of horizons viz apparent horizon and event horizon for the universe and using first law of thermodynamics, we have examined the validity of GSL on both apparent and event horizons. Next, we have considered two types of entropy-corrections on apparent and event horizons. Using the modified area law, we have examined the validity of GSL of thermodynamics on apparent and event horizons under some restrictions of model parameters. (orig.)

  12. The rotating scalar field vacuum on anti-de Sitter space-time

    CERN Document Server

    Kent, Carl

    2015-01-01

    We consider the definition of the vacuum state of a quantum scalar field on $n$-dimensional anti-de Sitter space-time as seen by an observer rotating about the polar axis. Since positive (or negative) frequency scalar field modes must have positive (or negative) Klein-Gordon norm respectively, we find that the only sensible choice of positive frequency corresponds to positive frequency as seen by a static observer. This means that the rotating vacuum is identical to the nonrotating vacuum. If the angular velocity of the rotating observer is smaller than the inverse of the anti-de Sitter radius of curvature, then modes with positive Klein-Gordon norm also have positive frequency as seen by the rotating observer. We comment on the implications of this result for the construction of rotating thermal states.

  13. The M-sigma Relation of Super Massive Black Holes from the Scalar Field Dark Matter

    CERN Document Server

    Lee, Jae-Weon; Kim, Hyeong-Chan

    2015-01-01

    We explain the M-sigma relation between the mass of super massive black holes in galaxies and the velocity dispersions of their bulges in the scalar field or the Bose-Einstein condensate dark matter model. The gravity of the central black holes changes boundary conditions of the scalar field at the galactic centers. Owing to the wave nature of the dark matter this significantly changes the galactic halo profiles even though the black holes are much lighter than the bulges. As a result the heavier the black holes are, the more compact the bulges are, and hence the larger the velocity dispersions are. This tendency is verified by a numerical study. The M-sigma relation is well reproduced with the dark matter particle mass $m\\simeq 5\\times 10^{-22} eV$.

  14. Future evolution in a backreaction model and the analogous scalar field cosmology

    CERN Document Server

    Ali, Amna

    2016-01-01

    We investigate the future evolution of the universe using the Buchert framework for averaged backreaction in the context of a two-domain partition of the universe. We show that this approach allows for the possibility of the global acceleration vanishing at a finite future time, provided that none of the subdomains accelerate individually. The model at large scales is analogously described in terms of a homogeneous scalar field emerging with a potential that is fixed and free from phenomenological parametrization. The dynamics of this scalar field is explored in the analogous FLRW cosmology. We use observational data from Type Ia Supernovae, Baryon Acoustic Oscillations, and Cosmic Microwave Background to constrain the parameters of the model for a viable cosmology, providing the corresponding likelihood contours.

  15. Scalar field as a Bose-Einstein condensate in a Schwarzschild-de Sitter spacetime

    CERN Document Server

    Castellanos, Elías; Lämmerzahl, Claus; Macías, Alfredo

    2015-01-01

    In this paper we analyze some properties of a scalar field configuration, where it is considered a trapped Bose-Einstein condensate in a Schwarzschild-de Sitter background spacetime. In a natural way, the geometry of the curved spacetime provides an effective trapping potential for the scalar field configuration. This fact allows to explore some thermodynamical properties of the system. Additionally, the curved geometry of the spacetime also induces a position dependent self-interaction parameter, that can be interpreted as a kind of \\emph{gravitational Feshbach resonance}, which could affect the stability of the \\emph{cloud} and could be used to obtain information about the interactions among the components of the system.

  16. Resonant frequencies of massless scalar field in rotating black-brane spacetime

    Institute of Scientific and Technical Information of China (English)

    Jing Ji-Liang; Pan Qi-Yuan

    2008-01-01

    This paper investigates the resonant frequencies of the massless scalar field in the near extremal Kerr-like black-brahe spacetime. It is shown that the different angular quantum number will present different resonant frequencies. It is also shown that the real part of the resonant frequencies increases as the compact dimensions parameter μi increases, but the magnitude of the imaginary part decreases as μi increases.

  17. On the critical behaviour of the 2-point function in scalar field theories

    Energy Technology Data Exchange (ETDEWEB)

    Malbouisson, A.P.C. [Centro Brasileiro de Pesquisas Fisicas (CBPF), Rio de Janeiro, RJ (Brazil)

    1999-09-01

    By the use of a Mellin representation of Feynman integrals, a convergent asymptotic expansion for generic Feynman amplitudes for any set of invariants going to zero or to {infinity}, may be obtained. In the case of scalar field theories in Euclidean metric, we use this expansion to analyse the behaviour of the two-point function for small values of the mass parameter, for fixed external momentum. (author)

  18. A topological state sum model for a scalar field on the circle

    CERN Document Server

    Kerr, Steven

    2016-01-01

    This paper is a follow-up to a previous paper on fermions. A simple state sum model for a scalar field on a triangulated 1-manifold is constructed. The model is independent of the triangulation and gives exactly the same partition function as the continuum functional integral with zeta function regularisation. For a certain choice of gauge group, the state sum model on the circle is equivalent to the path integral for the simple harmonic oscillator.

  19. Oscillons in Scalar Field Theories: Applications in Higher Dimensions and Inflation

    OpenAIRE

    Gleiser, Marcelo

    2006-01-01

    The basic properties of oscillons -- localized, long-lived, time-dependent scalar field configurations -- are briefly reviewed, including recent results demonstrating how their existence depends on the dimensionality of spacetime. Their role on the dynamics of phase transitions is discussed, and it is shown that oscillons may greatly accelerate the decay of metastable vacuum states. This mechanism for vacuum decay -- resonant nucleation -- is then applied to cosmological inflation. A new infl...

  20. Oscillons in Scalar Field Theories: Applications in Higher Dimensions and Inflation

    CERN Document Server

    Gleiser, M

    2006-01-01

    The basic properties of oscillons -- localized, long-lived, time-dependent scalar field configurations -- are briefly reviewed, including recent results demonstrating how their existence depends on the dimensionality of spacetime. Their role on the dynamics of phase transitions is discussed, and it is shown that oscillons may greatly accelerate the decay of metastable vacuum states. This mechanism for vacuum decay -- resonant nucleation -- is then applied to cosmological inflation. A new inflationary model is proposed which terminates with fast bubble nucleation.