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Sample records for algol

  1. Programming Algol

    CERN Document Server

    Malcolme-Lawes, D J

    2014-01-01

    Programming - ALGOL describes the basics of computer programming using Algol. Commands that could be added to Algol and could increase its scope are described, including multiplication and division and the use of brackets. The idea of labeling or naming a command is also explained, along with a command allowing two alternative results. Most of the important features of Algol syntax are discussed, and examples of compound statements (that is, sets of commands enclosed by a begin ... end command) are given.Comprised of 11 chapters, this book begins with an introduction to the digital computer an

  2. UXOR Hunting among Algol Variables

    Science.gov (United States)

    Poxon, M.

    2015-06-01

    The class of variable typified by UX Orionis (UXORs or UXors) are young stars characterised by aperiodic or semiperiodic fades from maximum. This has led to several of the class being formerly catalogued as Algol-type eclipsing binaries (EAs), which can show superficially similar light variations. With this in view, I propose a campaign to search for more UX Ori type stars.

  3. Accretion disks in Algols: progenitors and evolution

    CERN Document Server

    Van Rensbergen, W

    2016-01-01

    There are only a few Algols with measured accretion disk parameters. These measurements provide additional constraints for tracing the origin of individual systems, narrowing down the initial parameter space. We investigate the origin and evolution of 6 Algol systems with accretion disks to find the initial parameters and evolutionary constraints for them. With a modified binary evolution code, series of close binary evolution are calculated to obtain the best match for observed individual systems. Initial parameters for 6 Algol systems with accretion disks were determined matching both the present system parameters and the observed disk characteristics. When RLOF starts during core hydrogen burning of the donor, the disk lifetime was found to be short. The disk luminosity is comparable to the luminosity of the gainer during a large fraction of the disk lifetime.

  4. On extensions of ALGOL-like languages

    DEFF Research Database (Denmark)

    Skyum, Sven

    1974-01-01

    In this paper we introduce the notion of a level grammar and a level language. We define an extension to the extended definable sets and we characterize ALGOL-like languages, extended definable sets, and extensions of those as languages generated by level grammars with different kinds of restrict......In this paper we introduce the notion of a level grammar and a level language. We define an extension to the extended definable sets and we characterize ALGOL-like languages, extended definable sets, and extensions of those as languages generated by level grammars with different kinds...

  5. Spectroscopically resolving the Algol triple system

    CERN Document Server

    Kolbas, V; Southworth, J; Lee, C -U; Lee, D -J; Lee, J W; Kim, S -L; Kim, H -I; Smalley, B; Tkachenko, A

    2015-01-01

    Algol ($\\beta$ Persei) is the prototypical semi-detached eclipsing binary and a hierarchical triple system. From 2006 to 2010 we obtained 121 high-resolution and high-S/N \\'{e}chelle spectra of this object. Spectral disentangling yields the individual spectra of all three stars, and greatly improved elements both the inner and outer orbits. We find masses of $M_{\\rm A} = 3.39\\pm0.06$ M$_\\odot$, $M_{\\rm B} = 0.770\\pm0.009$ M$_\\odot$ and $M_{\\rm C} = 1.58\\pm0.09$ M$_\\odot$. The disentangled spectra also give the light ratios between the components in the $B$ and $V$ bands. Atmospheric parameters for the three stars are determined, including detailed elemental abundances for Algol A and Algol C. We find the following effective temperatures: $T_{\\rm A} = 12\\,550\\pm120$ K, $T_{\\rm B} = 4900\\pm300$ K and $T_{\\rm C} = 7550\\pm250$ K. The projected rotational velocities are $v_{\\rm A} \\sin i_{\\rm A} = 50.8\\pm0.8$ km/s, $v_{\\rm B} \\sin i_{\\rm B} = 62\\pm2$ km/s and $v_{\\rm C} \\sin i_{\\rm C} = 12.4\\pm0.6$ km/s. This is t...

  6. Gas stream in Algol. [mass transfer in binary star systems

    Science.gov (United States)

    Cugier, H.; Chen, K.-Y.

    1977-01-01

    Additional absorption features in the red wings of the Mg II resonance lines near 2800 A are found in observations of Algol made from the Copernicus satellite. The absorption features were clearly seen only during a part of the primary eclipse, in the phase interval 0.90-0.03. The observations are interpreted as being produced by a stream of matter flowing from Algol B in the direction of Algol A. The measured Doppler shifts of the features give the value of 150 km/s as the characteristic velocity of matter in the stream. The mass transfer connected with the stream is estimated to be of the order of 10 to the -13th power solar mass per year.

  7. Numerical methods of mathematical optimization with Algol and Fortran programs

    CERN Document Server

    Künzi, Hans P; Zehnder, C A; Rheinboldt, Werner

    1971-01-01

    Numerical Methods of Mathematical Optimization: With ALGOL and FORTRAN Programs reviews the theory and the practical application of the numerical methods of mathematical optimization. An ALGOL and a FORTRAN program was developed for each one of the algorithms described in the theoretical section. This should result in easy access to the application of the different optimization methods.Comprised of four chapters, this volume begins with a discussion on the theory of linear and nonlinear optimization, with the main stress on an easily understood, mathematically precise presentation. In addition

  8. The Algol triple system spatially resolved at optical wavelengths

    CERN Document Server

    Zavala, R T; Boboltz, D A; Ojha, R; Shaffer, D B; Tycner, C; Richards, M T; Hutter, D J; 10.1088/2041-8205/715/1/L44

    2010-01-01

    Interacting binaries typically have separations in the milli-arcsecond regime and hence it has been challenging to resolve them at any wavelength. However, recent advances in optical interferometry have improved our ability to discern the components in these systems and have now enabled the direct determination of physical parameters. We used the Navy Prototype Optical Interferometer to produce for the first time images resolving all three components in the well-known Algol triple system. Specifically, we have separated the tertiary component from the binary and simultaneously resolved the eclipsing binary pair, which represents the nearest and brightest eclipsing binary in the sky. We present revised orbital elements for the triple system, and we have rectified the 180-degree ambiguity in the position angle of Algol C. Our directly determined magnitude differences and masses for this triple star system are consistent with earlier light curve modeling results.

  9. Doppler Shifts and Broadening and the Structure of the X-ray Emission from Algol

    CERN Document Server

    Chung, S M; Kashyap, V L; Lin, L W; Ratzlaff, P W; Chung, Sun Mi; Drake, Jeremy J.; Kashyap, Vinay L.; Lin, Li Wei; Ratzlaff, Peter W.

    2004-01-01

    In a study of Chandra High Energy Transmission Grating spectra of Algol, we clearly detect Doppler shifts caused by the orbital motion of Algol B. These data provide the first definitive proof that the X-ray emission of Algol is dominated by the secondary, in concordance with expectations that Algol A (B8) is X-ray dark. The measured Doppler shifts are slightly smaller than expected, implying an effective orbital radius of about 10 Rsolar, instead of 11.5 Rsolar for the Algol B center of mass. This could be caused by a small contribution of X-ray flux from Algol A (10-15%), possibly through accretion. The more likely explanation is an asymmetric corona biased toward the system center of mass by the tidal distortion of the surface of Algol B. Analysis of the strongest lines indicates excess line broadening of ~150 km/s above that expected from thermal motion and surface rotation. Possible explanations include turbulence, flows or explosive events, or rotational broadening from a radially extended corona. We fa...

  10. From the Heart of The Ghoul: C and N Abundances in the Corona of Algol B

    CERN Document Server

    Drake, J J

    2003-01-01

    Chandra Low Energy Transmission Grating Spectrograph observations of Algol have been used to determine the abundances of C and N in the secondary star for the first time. The analysis was performed relative to similar observations of an adopted "standard" star HR 1099. It is demonstrated that HR 1099 and Algol are coronal twins in many respects and that their X-ray spectra are very similar in nearly all details, except for the observed strengths of C and N lines. The H-like transitions of C and N in the coronae of Algol and HR 1099 demonstrate that the surface abundances of Algol B have been strongly modified by CN-processing, as shown earlier by Schmitt & Ness (2002). It is found that N is enhanced in Algol B by a factor of 3 compared to HR 1099. No C lines are detected in the Algol spectrum, indicating a C depletion relative to HR 1099 by a factor of 10 or more. These C and N abundances indicate that Algol B must have lost at least half of its initial mass, and are consistent with predictions of evoluti...

  11. Cyclic period changes in the algol ww cygni

    Directory of Open Access Journals (Sweden)

    R. T. Zavala

    2004-01-01

    Full Text Available Se han observado variaciones c clicas del per odo en muchas clases de binarias cercanas con una duraci on comprendida entre un a~no y una d ecada. WW Cygni, la binaria tipo Algol, presenta una variaci on c clica en su per odo orbital con una amplitud de algo m as de 0.02 d as y un per odo de 56 a~nos. Un tercer o cuarto cuerpo hipot etico no explica satisfactoriamente esta variaci on observada en su per odo orbital. Las variaciones en luminosidad y color del sistema en el m nimo primario del eclipse concuerdan con el modelo propuesto por Applegate para variaciones de per odo inducidas por el ciclo magn etico en WW Cygni. Hemos comenzado a realizar una serie de observaciones de 9 binarias cercanas para buscar evidencias de variaciones en luminosidad y color consistentes con la hip otesis del ciclo magn etico. Se sugiere Librae como un caso apropiado para realizar observaciones con un interfer ometro optico con el n de veri car la hip otesis del tercer cuerpo propuesta para este sistema tipo Algol.

  12. Radio Astrometry of the Triple Systems Algol and UX Arietis

    Science.gov (United States)

    Peterson, W. M.; Mutel, R. L.; Lestrade, J.-F.; Güdel, M.; Goss, W. M.

    2011-08-01

    We have used multi-epoch long-baseline radio interferometry to determine the proper motion and orbital elements of Algol and UX Arietis, two radio-bright, close binary stellar systems with distant tertiary components. For Algol, we refine the proper motion and outer orbit solutions, confirming the recent result of Zavala et al. that the inner orbit is retrograde. The radio centroid closely tracks the motion of the KIV secondary. In addition, the radio morphology varies from double-lobed at low flux level to crescent-shaped during active periods. These results are most easily interpreted as synchrotron emission from a large, co-rotating meridional loop centered on the K star. If this is correct, it provides a radio-optical frame tie candidate with an uncertainty ±0.5 mas. For UX Arietis, we find an outer orbit solution that accounts for previous very long baseline interferometry observations of an acceleration term in the proper motion fit. The outer orbit solution is also consistent with previously published radial velocity curves and speckle observations of a third body. The derived tertiary mass, 0.75 solar masses, is consistent with the K1 main-sequence star detected spectroscopically. The inner orbit solution favors radio emission from the active K0IV primary only. The radio morphology, consisting of a single, partially resolved emission region, may be associated with the persistent polar spot observed using Doppler imaging.

  13. A comprehensive study of six Algol type binaries

    CERN Document Server

    Liakos, Alexios; Niarchos, Panagiotis

    2014-01-01

    CCD light curves of the Algol type eclipsing binaries DP Cep, AL Gem, FG Gem, UU Leo, CF Tau and AW Vul were analysed using the Wilson-Deninney code and new geometric and absolute parameters were derived. Due to cyclic apparent orbital period changes of the systems, probably caused by the Light-Time Effect, the contribution of a third light was taken into account in the light curve solution. All the reliable timings of minima found in the literature were used to study the period variations and search for the presence of a tertiary component in the systems. A comparison between the parameters of the third body derived from the light curve and orbital period analyses is also discussed. Moreover, the absolute parameters of the eclipsing binary components were also used to determine their current evolutionary state.

  14. A comprehensive study of six Algol type binaries

    Science.gov (United States)

    Liakos, A.; Zasche, P.; Niarchos, P.

    2011-12-01

    CCD light curves of the Algol type eclipsing binaries DP Cep, AL Gem, FG Gem, UU Leo, CF Tau and AW Vul were analysed using the Wilson-Devinney code and new geometric and absolute parameters were derived. Due to cyclic apparent orbital period changes of the systems, probably caused by the Light-Time Effect, the contribution of a third light was taken into account in the light curve solution. All the reliable timings of minima found in the literature were used to study the period variations and search for the presence of a tertiary component in the systems. A comparison between the parameters of the third body derived from the light curve and orbital period analyses is also discussed. Moreover, the absolute parameters of the eclipsing binary components were also used to determine their current evolutionary state.

  15. Non-conservative evolution in Algols: where is the matter?

    CERN Document Server

    Deschamps, Romain; Jorissen, Alain; Siess, Lionel; Baes, Marteen; Camps, Peter

    2015-01-01

    There is gathering indirect evidence suggesting non-conservative evolutions in Algols. However, the systemic mass-loss rate is poorly constrained by observations and generally set as a free parameter in binary-star evolution simulations. Moreover, systemic mass loss may lead to observational signatures that are still to be found. We investigate the impact of the outflowing gas and the possible presence of dust grains on the spectral energy distribution (SED). We used the 1D plasma code Cloudy and compared the results with the 3D Monte-Carlo radiative transfer code Skirt for dusty simulations. The circumbinary mass-distribution and binary parameters are computed with state-of-the-art binary calculations done with the Binstar evolution code. The outflowing material reduces the continuum flux-level of the stellar SED in the optical and UV. Due to the time-dependence of this effect, it may help to distinguish between different ejection mechanisms. Dust, if present, leads to observable infrared excesses even with ...

  16. Shifting Milestones of Natural Sciences: The Ancient Egyptian Discovery of Algol's Period Confirmed

    CERN Document Server

    Jetsu, Lauri

    2016-01-01

    The Ancient Egyptians wrote Calendars of Lucky and Unlucky Days that assigned astronomically influenced prognoses for each day of the year. The best preserved of these calendars is the Cairo Calendar (hereafter CC) dated to 1244--1163 B.C. We have presented evidence that the 2.85 days period in the lucky prognoses of CC is equal to that of the eclipsing binary Algol during this historical era. We wanted to find out the vocabulary that represents Algol in the mythological texts of CC. Here we show that Algol was represented as Horus and thus signified both divinity and kingship. The texts describing the actions of Horus are consistent with the course of events witnessed by any naked eye observer of Algol. These descriptions support our claim that CC is the oldest preserved historical document of the discovery of a variable star. The period of the Moon, 29.6 days, has also been discovered in CC. We show that the actions of Seth were connected to this period, which also strongly regulated the times described as ...

  17. Shifting Milestones of Natural Sciences: The Ancient Egyptian Discovery of Algol's Period Confirmed

    Science.gov (United States)

    Jetsu, Lauri; Porceddu, Sebastien

    2015-12-01

    The Ancient Egyptians wrote Calendars of Lucky and Unlucky Days that assigned astronomically influenced prognoses for each day of the year. The best preserved of these calendars is the Cairo Calendar (hereafter CC) dated to 1244-1163 B.C. We have presented evidence that the 2.85 days period in the lucky prognoses of CC is equal to that of the eclipsing binary Algol during this historical era. We wanted to find out the vocabulary that represents Algol in the mythological texts of CC. Here we show that Algol was represented as Horus and thus signified both divinity and kingship. The texts describing the actions of Horus are consistent with the course of events witnessed by any naked eye observer of Algol. These descriptions support our claim that CC is the oldest preserved historical document of the discovery of a variable star. The period of the Moon, 29.6 days, has also been discovered in CC. We show that the actions of Seth were connected to this period, which also strongly regulated the times described as lucky for Heaven and for Earth. Now, for the first time, periodicity is discovered in the descriptions of the days in CC. Unlike many previous attempts to uncover the reasoning behind the myths of individual days, we discover the actual rules in the appearance and behaviour of deities during the whole year.

  18. A search for systemic mass loss in Algols with bow shocks

    CERN Document Server

    Mayer, Andreas; Jorissen, Alain

    2016-01-01

    Aims. Various studies indicate that interacting binary stars of Algol type evolve non-conservatively. However, direct detection of systemic mass loss in Algols has been scarce so far. We aim at studying the systemic mass loss in Algols by looking for the presence of infrared excesses originating from the thermal emission of dust grains, which is linked to the presence of a stellar wind. Methods. In contrast to previous studies, we make use of the fact that stellar and interstellar material is piled up at the edge of the asterosphere where the stellar wind interacts with the interstellar medium. We analyse WISE W3 $12\\,\\mu$m and WISE W4 $22\\,\\mu$m data of Algol-type binary Be and B[e] stars and the properties of their bow shocks. From the stand-off distance of the bow shock we are able to determine the mass loss rate of the binary system. Results. Although the velocities of the stars with respect to the interstellar medium are quite low, we find bow shocks to be present in two systems, namely $\\pi$ Aqr, and $\\...

  19. TYC 4031-791-1 - a new eclipsing binary of Algol type

    Science.gov (United States)

    Galan, C.; Tomov, T.; Swierczynski, E.; Wychudzki, P.; Brozek, T.; Ilkiewicz, K.; Mikolajewski, M.; Drozd, K.

    2012-06-01

    We report on the discovery of TYC 4031-791-1 as an eclipsing binary of Algol type which shows primary and secondary eclipses with period P_orb approx. 6.68 days. The system is composed of two, perhaps similar stars of spectral type around B5 on slightly eccentric orbit.

  20. INTERACTING BINARY STARS ENVIRONMENTS AND THE W SER-DPV-ALGOL CONNECTION

    Directory of Open Access Journals (Sweden)

    R. E. Mennickent

    2010-01-01

    Full Text Available Revisamos el trabajo reciente en algunos campos de binarias interactuantes con énfasis en Variables Cata- clásmicas, tipo Algol y Variables de Doble Periodo (DPVs. La secuencia de sistemas W Serpentis (muymasivas con variabilidad irregular y gran pérdida de masa ! DPVs (menos masivas con variabilidad regular y pérdida de masa cíclica ! Algoles (aún menos masivas con poca pérdida de masa podría corresponder a una secuencia evolutiva e ilustrar la importancia de la tasa de intercambio de masa en determinar las propiedades observables y de pérdida de masa de estos sistemas.

  1. Binary evolution using the theory of osculating orbits: conservative Algol evolution

    CERN Document Server

    Davis, P J; Deschamps, R

    2014-01-01

    Our aim is to calculate the evolution of Algol binaries within the framework of the osculating orbital theory, which considers the perturbing forces acting on the orbit of each star arising from mass exchange via Roche lobe overflow (RLOF). The scheme is compared to results calculated from a `classical' prescription. Using our stellar binary evolution code BINSTAR, we calculate the orbital evolution of Algol binaries undergoing case A and case B mass transfer, by applying the osculating scheme. The velocities of the ejected and accreted material are evaluated by solving the restricted three-body equations of motion, within the ballistic approximation. This allows us to determine the change of linear momentum of each star, and the gravitational force applied by the mass transfer stream. Torques applied on the stellar spins by tides and mass transfer are also considered. Using the osculating formalism gives shorter post-mass transfer orbital periods typically by a factor of 4 compared to the classical scheme, o...

  2. Short period light variation of the Algol-type binary U Coronae Borealis

    Science.gov (United States)

    Narusawa, Shin-Ya; Waki, Yoshifumi; Ioroi, Masayuki; Nakamura, Yasuhisa; Takeuti, Mine

    The short period variability in the light curve of U CrB, an Algol-type binary, was examined with the published data of van Gent (1989). The period of variability was approximately 0.05 d and the amplitude was 0.05 mag. The superposition of several modes was suggested. The properties of the light variability were compared with those of the early-type main-sequence pulsating stars.

  3. Continuous heating of a giant X-ray flare on Algol

    CERN Document Server

    Schmitt, J H M M

    1999-01-01

    Giant flares can release large amounts of energy within a few days: X-ray emission alone can be up to ten percent of the star's bolometric luminosity. These flares exceed the luminosities of the largest solar flares by many orders of magnitude, which suggests that the underlying physical mechanisms supplying the energy are different from those on the Sun. Magnetic coupling between the components in a binary system or between a young star and an accretion disk has been proposed as a prerequisite for giant flares. Here we report X-ray observations of a giant flare on Algol B, a giant star in an eclipsing binary system. We observed a total X-ray eclipse of the flare, which demonstrates that the plasma was confined to Algol B, and reached a maximum height of 0.6 stellar radii above its surface. The flare occurred around the south pole of Algol B, and energy must have been released continously throughout its life. We conclude that a specific extrastellar environment is not required for the presence of a flare, and...

  4. Photometric Properties for Selected Algol-type Binaries. V. V1241 Tauri

    Science.gov (United States)

    Yang, Y.-G.; Zhang, X.-B.; Li, H.-L.; Dai, H.-F.

    2012-11-01

    We present new photometry for the eclipsing binary V1241 Tau, which was obtained on six nights between 2011 December and 2012 January using the 85 cm telescope at the Xinglong station of the National Astronomical Observatories of China. By using the updated Wilson-Devinney code, photometric models with third lights were deduced from two sets of light curves. The result implies that V1241 Tau is an Algol-type near-contact binary (NCB), whose mass ratio and filling-out of the primary are q = 0.545 (± 0.003) and f 1 = 82.4% (± 0.2%), respectively. Based on all available times of minimum light spanning over 80 yr, the O - C curve of V1241 Tau appears to show a quasi-sinusoidal oscillation, i.e., a light-time orbit. The modulated period and amplitude are P mod = 47.4 (± 1.7) yr and A = 0.0087 (± 0.0005) days, respectively. This kind of period variation may be more likely attributed to the light-time effect via a presence of an unseen third body. From an analysis of 23 Algol-type NCBs with EB-type light curves, we determine that the fill-out for the primary f 1 will increase as the orbital period P decreases. With angular momentum loss, the orbit of the binary will shrink, which causes f 1 to increase. The primary component finally fills its Roche lobe, and the binary evolves into contact configuration. Therefore, this kind of Algol-type NCB with EB-type light curves, such as V1241 Tau, may be a progenitor of the A-type W UMa binary.

  5. The Algol-Type Eclipsing Binary X Tri: BVRI modeling and O-C Diagram Analysis

    Science.gov (United States)

    Liakos, A.; Zasche, P.; Niarchos, P.

    2010-12-01

    CCD photometric observations of the Algol-type eclipsing binary X Tri have been obtained. The light curves are analyzed with the Wilson-Devinney (WD) code and new geometric and photometric elements are derived. A new O-C analysis of the system, based on the most reliable timings of minima found in the literature, is presented and apparent period changes are discussed with respect to possible and multiple Light-Time Effect (LITE) in the system. Moreover, the results for the existence of additional bodies around the eclipsing pair, derived from the period study, are compared with those for extra luminosity, derived from the light curve analysis.

  6. The Algol type eclipsing binary X Tri: BVRI modelling and O-C diagram analysis

    CERN Document Server

    Liakos, A; Niarchos, P

    2009-01-01

    CCD photometric observations of the Algol-type eclipsing binary X Tri have been obtained. The light curves are analyzed with the Wilson-Devinney (WD) code and new geometric and photometric elements are derived. A new O-C analysis of the system, based on the most reliable timings of minima found in the literature, is presented and apparent period changes are discussed with respect to possible and multiple Light-Time Effect (LITE) in the system. Moreover, the results for the existence of additional bodies around the eclipsing pair, derived from the period study, are compared with those for extra luminosity, derived from the light curve analysis.

  7. Orbital period variation study of the low-mass Algol eclipsing binary AI Draconis

    Directory of Open Access Journals (Sweden)

    Magdy A. Hanna

    2013-06-01

    Full Text Available Orbital period changes for the Algol-type eclipsing binary AI Dra were studied based on the analysis of its observed times of light minimum. The period variation showed cyclic changes in the interval from JD. ≈ 2436000 to JD. ≈ 2447500 and a secular period increase rate (dP/dt = 2.44 × 10−7 d/year starting from JD. ≈ 2448500 up to 2455262, in a time scale equals to 5 × 106 year.

  8. A Hot Spot and Mass Transfer of the Algol-type Binary System WZ Crv

    CERN Document Server

    Virnina, Natalia A; Mogorean, Maxim V

    2011-01-01

    We present the results of two color VR observation of the Algol-type binary system WZ Crv (12h44m15.19s, -21d25m35.4s) which were obtained using the remotely controlled telescope TOA-150 of Tzec Maun Observatory. We determined the moments of individual minima, the orbital period and its derivative, the initial epoch, color indices V-R and temperature estimates of the components. Also we noticed that the phase curve is asymmetric: the second maximum is higher than the first one. It indicates that there is a spot in the photosphere of one of the stars in this system.

  9. TZ Lyrae: an Algol-type Eclipsing Binary with Mass Transfer

    Science.gov (United States)

    Yang, Yuan-Gui; Yin, Xin-Guo

    2007-04-01

    We present a detailed investigation of the Algol-type binary TZ Lyrae, based on 55 light minimum timings spanning 90 years. It is found that the orbital period shows a long-term increase with a cyclic variation superimposed. The rate of the secular increase is dP/dt=+7.18× 10^{-8} d yr^{-1}, indicating that a mass transfer from the less massive component to the more massive one at a rate of dm=+2.21×10^{-8} M_⊙ yr^{-1}. The cyclic component, with a period of P_{3}=45.5 yr and an amplitude of A=0.0040°, may be interpreted as either the light-time effect in the presence of a third body or magnetic activity cycles in the components. Using the latest version Wilson-Devinney code, a revised photometric solution was deduced from B and V observations. The results show that TZ Lyr is an Algol-type eclipsing binary with a mass ratio of q=0.297(±0.003). The semidetached configuration with a lobe-filling secondary suggests a mass transfer from the secondary to the primary, which is in agreement with the long-term period increase of the binary system.

  10. The low-mass classic Algol-type binary UU Leo revisited

    Science.gov (United States)

    Yang, Yuan-Gui

    2013-12-01

    New multi-color photometry of the eclipsing binary UU Leo, acquired from 2010 to 2013, was carried out by using the 60-cm and 85-cm telescopes at the Xinglong station, which is administered by National Astronomical Observatories, Chinese Academy of Sciences. With the updated Wilson-Devinney code, the photometric solution was derived from BVR light curves. The results imply that UU Leo is a semi-detached Algol-type binary, with a mass ratio of q = 0.100(±0.002). The change in orbital period was reanalyzed based on all available eclipsing times. The O - C curve could be described by an upward parabola superimposed on a quasi-sinusoidal curve. The period and semi-amplitudes are Pmod = 54.5(±1.1) yr and A = 0.0273d(±0.0015d), which may be attributed to the light-time effect via the presence of an invisible third body. The long-term period increases at a rate of dP/dt = +4.64(±0.14) × 10-7d yr-1, which may be interpreted by the conserved mass being transferred from the secondary to the primary. With mass being transferred, the low-mass Algol-type binary UU Leo may evolve into a binary system with a main sequence star and a helium white dwarf.

  11. TZ Lyrae: an Algol-type Eclipsing Binary with Mass Transfer

    Institute of Scientific and Technical Information of China (English)

    Yuan-Gui Yang; Xin-Guo Yin

    2007-01-01

    We present a detailed investigation of the Algol-type binary TZ Lyrae, based on 55 light minimum timings spanning 90 years. It is found that the orbital period shows a long-term increase with a cyclic variation superimposed. The rate of the secular increase is dP/dt =+7.18 × 10-8d yr-1, indicating that a mass transfer from the less massive component to the more massive one at a rate of dm = +2.21 × 10-8M⊙ yr-1. The cyclic component, with a period of P3= 45.5 yr and an amplitude of A = 0d.0040, may be interpreted as either the light-time effect in the presence of a third body or magnetic activity cycles in the components.Using the latest version Wilson-Devinney code, a revised photometric solution was deduced from B and V observations. The results show that TZ Lyf is an Algol-type eclipsing binary with a mass ratio of q = 0.297(±0.003). The semidetached configuration with a lobe-filling secondary suggests a mass transfer from the secondary to the primary, which is in agreement with the long-term period increase of the binary system.

  12. Algol-like Interacting Binaries with Long Non-orbital Periodicities

    Science.gov (United States)

    Mennickent, R. E.

    The phenomenon of Double Periodic Variables (DPVs) is summarized, enlightening their photometric and spectroscopic characteristics. The current evidence for binarity, accretion discs and inflows/outflows is presented. Stellar masses, radii, temperature and luminosities, along with orbital and disc parameters, have been obtained for some systems as the result of a multicomponent fit to the light curves. These parameters have been compared with those of published binary star evolutionary tracks obtaining the best synthetic model for those systems. This allow us to discuss their evolutionary stage determining their age and mass transfer rate, and explore the possible relation between DPVs, W Serpentids and classical Algols. We provide clues on the origin of the long-term variability, mainly based on spectroscopic studies and photometric insights.

  13. Spectroscopic Evidence of Sporadic Gas Accretion onto the Herbig AE Stars with Non-Periodic Algol-Type Minima

    Science.gov (United States)

    Kozlova, O. V.; Grinin, V. P.; Rostopchina, A. N.

    We present the results of simultaneous spectroscopic and photometric observations for six isolated Herbig Ae stars with non-periodic Algol-like minima: UX Ori, BF Ori, CQ Tau, SV Cep, VX Gas, and WW Vul. In all cases the Ha line has the profile typical for axially symmetric accretion. In the spectra of five stars (CQ Tau is the exception) the strong He I 5876 Å line has been observed in absorption which is not typical of normal A stars. In three cases: UX Ori, VX Cas, and WW Vul, variability of this line is found. We did not observe any correlation between the strength of this line and the brightness of the stars. These observational facts are considered as evidence for gas accretion, which is probably an important property of young stars with non-periodic Algol-type minima.

  14. Three-Dimensional Hydrodynamic Simulations of Accretion in Short Period Algols

    CERN Document Server

    Raymer, Eric

    2012-01-01

    Recent observations have shown that the direct-impact Algol systems U CrB and RS Vul possess gas located outside of the orbital plane, including a tilted accretion disc in U CrB. Observations of circumstellar gas surrounding the mass donor in RS Vul suggest magnetic effects could be responsible for deflecting the accretion stream out of the orbital plane, resulting in a tilted disc. To determine whether a tilted disc is possible due to a deflected stream, we use three-dimensional hydrodynamic simulations of the mass transfer process in RS Vul. By deflecting the stream 45 degrees out of the orbital plane and boosting the magnitude of the stream's velocity to Mach 30, we mimic the effects of magnetic activity near L1. We find that the modified stream parameters change the direct-impact nature of the system. The stream misses the surface of the star, and a slightly warped accretion disc forms with no more than 3 degrees of disc tilt. The stream-disc interaction for the deflected stream forces a large degree of m...

  15. Photometric Study of the near-contact short period Algol system, AK Canis Minoris

    Science.gov (United States)

    Samec, Ronald G.; McDermith, Richard J.; Gray, Jamison D.; Carrigan, Brian

    1995-05-01

    As a part of our departments new undergraduate research program, we are surveying the eccentric eclipsing binary (EEB) candidates of Hegedus (1988). AK CMi is listed as a system with a displaced secondary. The observations were taken 10 to 15 February 1994, inclusive, at Lowell Obsevatory, Flagstaff, Arizona. A thermoelectrically cooled EMI 6256S ( S-13 cathode) PMT was used in conjunction with the 0.78 m National Undergraduate Research Observatory reflector. Two precision epochs of minimicrons light were determined from the observations made during primary and secondary eclipses. They are: Min I = 2449396.7032(5) and Min II = 2449395.8546(3). Targeting the last twenty-three years of data, we calculated improved linear and quadratic ephemerides. The quadratic term, -1.0(2)E-10, suggests that AK CMi is undergoing a continuous period decrease. This may be due to magnetic braking arising from the fast rotating solar-type secondary component. There is little evidence from the present light curves that AK CMi has a eccentric orbit. Assymetries near secondary minima possibly induced by an intermittent gas stream may be responsible for the classification of AK CMi as an EEB. The light curve solution reveals that AK CMi is a short period Algol with an A spectral-type primary component and an early K-type secondary. We calculated mass ratio of 0.5 and a secondary component fillout of 90% showing that AK CMi is a near contact binary.

  16. Orbital Solutions and Absolute Elements of the Massive Algol Binary ET Tauri

    Science.gov (United States)

    Williamon, Richard M.; Dale, Horace; Evavold, Charles L.; Langoussis, Alexander; Fekel, Francis C.; Muterspaugh, Matthew W.; Williams, Stephen; Napier, Kate; Sowell, James R.

    2016-12-01

    We acquired differential UBV photoelectric photometry and radial velocities of the relatively bright, understudied, massive Algol binary ET Tau and utilized the Wilson-Devinney (WD) analysis program to obtain a simultaneous solution of these observations. To improve the orbital ephemeris, the V measurements from the ASAS program were also analyzed. Because of the very rapid rotation of the significantly more massive and hotter component (B2/3 spectral class), only radial velocities of the secondary component, which has a ˜B7 spectral class, could be measured. We derive masses of {M}1=14.34+/- 0.28 {M}⊙ and {M}2=6.339+/- 0.117 {M}⊙ and equal-volume radii of {R}1=6.356+/- 0.056 {R}⊙ and {R}2=11.84+/- 0.10 {R}⊙ for the primary and secondary, respectively. The secondary is filling its Roche lobe, so the system is semi-detached. The effective temperature of the secondary was held fixed at 15,000 K, and the primary's temperature was found to be {30,280}+/- 109 K. The system, which has a period of 5.996883 ± 0.000002 days, is assumed to have a circular orbit and is seen at an inclination of 79\\buildrel{\\circ}\\over{.} 55+/- 0\\buildrel{\\circ}\\over{.} 05.

  17. Photometric Properties of Selected Algol-type Binaries. IX. V548 Cygni

    Science.gov (United States)

    Yang, Yuan-Gui; Wu, Chao; Van Hamme, W.; Hu, J.-Y.; Wei, J.-Y.

    2016-08-01

    We present a new UV light curve of the Algol eclipsing binary V548 Cyg obtained with the Lunar Ultraviolet Telescope. We model the UV light curve together with two previously published (B and V) light curves, primary star radial velocities, and eclipse timings in a unified multi-data-type solution and determine orbital parameters and absolute dimensions. Timing residuals hint at the presence of a third star in the system. This star is possibly the source of the third light that is needed to obtain a good fit to each of the light curves simultaneously. The light-time oscillation in the timing residuals has a period of either ≈ 19 or ≈ 46 years. The third body orbit inclination would have to be low (23^\\circ or 15^\\circ , respectively) for the third star to have a mass of ≈ 1.5 {M}⊙ , which would be expected for a main-sequence star of color B-V≈ 0.32, as determined from the light curve solution. In an H-R diagram, the mass-gaining, primary component of V548 Cyg is located between the zero-age and terminal-age main sequence for solar composition stars, and close to the 0.4 Gyr isochrone.

  18. Tracing CNO exposed layers in the Algol-type binary system u Her

    CERN Document Server

    Kolbas, V; Pavlovski, K; Southworth, J

    2014-01-01

    The chemical composition of stellar photospheres in mass-transferring binary systems is a precious diagnostic of the nucleosynthesis processes that occur deep within stars, and preserves information on the components history. The binary system u Her belongs to a group of hot Algols with both components being B-stars. We have isolated the individual spectra of the two components by the technique of spectral disentangling of a new series of 43 high-resolution echelle spectra. Augmenting these with an analysis of the Hipparcos photometry of the system yields revised stellar quantities for the components of u Her. For the primary component (the mass-gaining star) we find M_A = 7.88 +/- 0.26 M_sun, R_A = 4.93 +/- 0.15 R_sun and T_eff_A = 21600 +/- 220 K. For the secondary (the mass-losing star) we find M_B = 2.79 +/- 0.12 M_sun, R_B = 4.26 +/- 0.06 R_sun and T_eff_B = 12600 +/- 550 K. A non-LTE analysis of the primary star's atmosphere reveals deviations in the abundances of nitrogen and carbon from the standard c...

  19. Photometric properties for selected Algol-type binaries. VII. V404 and with magnetic activity

    Energy Technology Data Exchange (ETDEWEB)

    Zhang, Li-Yun; Pi, Qing-Feng; Zhu, Zhongzhong [College of Science/Department of Physics and NAOC-GZU Center for Astronomy, Guizhou University, Guiyang 550025 (China); Yang, Yuan-Gui, E-mail: liy_zhang@hotmail.com [School of Physics and Electronic Information, Huaibei Normal University, Huaibei 235000 Anhui Province (China)

    2014-03-01

    We present new CCD light curves of the short-period Algol-type eclipsing binary V404 And obtained in 2009-2011. The time-resolving multiple BVRI color light curves of the year 2011 with full phase coverage were analyzed simultaneously using the latest Wilson-Devinney program. We concluded that the configuration of two starspots on the primary is the most reliable explanation for the light curve distortions observed in 2011. Based on the new photometric solution, we further applied the spot model to explain the other light curves, including the previously published R-band light curves. We revealed that the starspots changed on a long timescale in terms of the spot parameters and the differences between Max. I and Max. II. Moreover, the O – C diagram spanning about 15 yr shows an upward parabola, which indicates a secular increase in the orbital period of V404 And. The orbital period increases at a rate of dP/dt = 5.3(0.3) × 10{sup –7} days yr{sup –1}, which might be interpreted by the angular momentum exchange via magnetic activity.

  20. Photometric Properties for Selected Algol-type Binaries. IV. AV Hydrae and DZ Cassiopeiae

    Science.gov (United States)

    Yang, Y.-G.; Li, L.-H.; Dai, H.-F.

    2012-08-01

    We present BVR photometric observations and several eclipsing times for AV Hya and DZ Cas from 2004 to 2011. Using the Wilson-Devinney method, the photometric solutions with hot spots were deduced from their asymmetric light curves. The results indicate that both stars are Algol-type binaries, whose mass ratio, q ph, and fill-out factor of the primary, f 1, are q ph = 0.255(± 0.002) and f 1 = 81.2(± 0.2)% for AV Hya, and q ph = 0.093(± 0.003) and f 1 = 98.7(± 0.3)% for DZ Cas. Based on all available light minimum times, it is discovered that the O - C curve of each star could be described by a light-time orbit overlying on a downward parabola. Their periods and amplitudes are P 3 = 37.2(± 0.7) yr and A = 0fd0095(±0fd0006) for AV Hya, and P 3 = 62.5(± 1.0) yr and A = 0fd0183(±0fd0007) for DZ Cas. Cyclic variations may result from the light-time effect due to the third body. The secular period decrease rates are dP/dt = -1.47(± 0.04) × 10-7 days yr-1 for AV Hya and dP/dt = -0.92(± 0.04) × 10-7 days yr-1 for DZ Cas. This may be interpreted using mass and angular momentum loss from the system. With decreasing period, the fill-out factor of the primary increases and it may finally fill its inner Roche lobe. Therefore, AV Hya and DZ Cas with a secular period decrease will evolve from semi-detached configurations into contact ones.

  1. PHOTOMETRIC PROPERTIES FOR SELECTED ALGOL-TYPE BINARIES. IV. AV HYDRAE AND DZ CASSIOPEIAE

    Energy Technology Data Exchange (ETDEWEB)

    Yang, Y.-G.; Dai, H.-F. [School of Physics and Electronic Information, Huaibei Normal University, 235000 Huaibei, Anhui Province (China); Li, L.-H., E-mail: yygcn@163.com [National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing (China)

    2012-08-15

    We present BVR photometric observations and several eclipsing times for AV Hya and DZ Cas from 2004 to 2011. Using the Wilson-Devinney method, the photometric solutions with hot spots were deduced from their asymmetric light curves. The results indicate that both stars are Algol-type binaries, whose mass ratio, q{sub ph}, and fill-out factor of the primary, f{sub 1}, are q{sub ph} = 0.255({+-} 0.002) and f{sub 1} = 81.2({+-} 0.2)% for AV Hya, and q{sub ph} = 0.093({+-} 0.003) and f{sub 1} = 98.7({+-} 0.3)% for DZ Cas. Based on all available light minimum times, it is discovered that the O - C curve of each star could be described by a light-time orbit overlying on a downward parabola. Their periods and amplitudes are P{sub 3} = 37.2({+-} 0.7) yr and A = 0fd0095({+-}0fd0006) for AV Hya, and P{sub 3} = 62.5({+-} 1.0) yr and A = 0fd0183({+-}0fd0007) for DZ Cas. Cyclic variations may result from the light-time effect due to the third body. The secular period decrease rates are dP/dt = -1.47({+-} 0.04) Multiplication-Sign 10{sup -7} days yr{sup -1} for AV Hya and dP/dt = -0.92({+-} 0.04) Multiplication-Sign 10{sup -7} days yr{sup -1} for DZ Cas. This may be interpreted using mass and angular momentum loss from the system. With decreasing period, the fill-out factor of the primary increases and it may finally fill its inner Roche lobe. Therefore, AV Hya and DZ Cas with a secular period decrease will evolve from semi-detached configurations into contact ones.

  2. An orbital period investigation of the Algol-type eclipsing binary VW Hydrae

    Institute of Scientific and Technical Information of China (English)

    Jia Zhang; Sheng-Bang Qian; Boonrucksar Soonthornthum

    2009-01-01

    Orbital period variations of the Algol-type eclipsing binary, VW Hydrae, are analyzed based on one newly determined eclipse time and the other times of light minima collected from the literature. It is discovered that the orbital period shows a continuous increase at a rate of dP/dt = +6.34×10-7 d yr-1 while it undergoes a cyclic change with an amplitude of 0.0639 d and a period of 51.5 yr. After the long-term period increase and the large-amphtude period oscillation were subtracted from the O-C curve, the residuals of the photoelectric and CCD data indicate a small-amplitude cyclic variation with a period of 8.75 yr and a small amplitude of 0.0048d. The continuous period increase indicates a conservative mass transfer at a rate of dM2/dt = 7.89×10-8 M⊙ yr-1 from the secondary to the primary. The period increase may be caused by a combination of the mass transfer from the secondary to the primary and the angular momentum transfer from the binary system to the circumbinary disk. The two cyclic period oscillations can be explained by light-travel time effects via the presence of additional bodies. The small-amplitude periodic change indicates the existence of a less massive component with mass M3 > 0.53 M⊙, while the large-amplitude one is caused by the presence of a more massive component with mass M4 > 2.84 M⊙. The ultraviolet source in the system reported by Kviz & Rufener (1987) may be one of the additional components, and it is possible that the more massive one may be an unseen neutron star or black hole. The rapid period increase and the possibility of the presence of two additional components in the binary make it a very interesting system to study. New photometric and high-resolution spectroscopic observations and a detailed investigation of those data are required in the future.

  3. LUT REVEALS AN ALGOL-TYPE ECLIPSING BINARY WITH THREE ADDITIONAL STELLAR COMPANIONS IN A MULTIPLE SYSTEM

    Energy Technology Data Exchange (ETDEWEB)

    Zhu, L.-Y.; Zhou, X.; Qian, S.-B.; Li, L.-J.; Liao, W.-P.; Tian, X.-M.; Wang, Z.-H. [Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, 650011 Kunming (China); Hu, J.-Y., E-mail: zhuly@ynao.ac.cn [National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing (China)

    2016-04-15

    A complete light curve of the neglected eclipsing binary Algol V548 Cygni in the UV band was obtained with the Lunar-based Ultraviolet Telescope in 2014 May. Photometric solutions are obtained using the Wilson–Devinney method. It is found that solutions with and without third light are quite different. The mass ratio without third light is determined to be q = 0.307, while that derived with third light is q = 0.606. It is shown that V548 Cygni is a semi-detached binary where the secondary component is filling the critical Roche lobe. An analysis of all available eclipse times suggests that there are three cyclic variations in the O–C diagram that are interpreted by the light travel-time effect via the presence of three additional stellar companions. This is in agreement with the presence of a large quantity of third light in the system. The masses of these companions are estimated as m sin i′ ∼ 1.09, 0.20, and 0.52 M{sub ⊙}. They are orbiting the central binary with orbital periods of about 5.5, 23.3, and 69.9 years, i.e., in 1:4:12 resonance orbit. Their orbital separations are about 4.5, 13.2, and 26.4 au, respectively. Our photometric solutions suggest that they contribute about 32.4% to the total light of the multiple system. No obvious long-term changes in the orbital period were found, indicating that the contributions of the mass transfer and the mass loss due to magnetic braking to the period variations are comparable. The detection of three possible additional stellar components orbiting a typical Algol in a multiple system make V548 Cygni a very interesting binary to study in the future.

  4. Period studies of classical Algol-type binaries II: UX Leo, RW Mon, EQ Ori, XZ UMa and AX Vul

    Science.gov (United States)

    Soydugan, F.; Erdem, A.; Doğru, S. S.; Aliçavuş, F.; Soydugan, E.; Çiçek, C.; Demircan, O.

    2011-07-01

    This study presents an investigation of the orbital period variations of five Algol type binaries, UX Leo, RW Mon, EQ Ori, XZ UMa and AX Vul based on all available minima times. The O- C diagrams of all systems exhibit a periodic variation superimposed on a downward parabolic segment. The mass loss due to magnetic braking effect in the cooler components is assumed to account for the parabolic variation with a downward shape, while it is suggested that the light-time effect (LITE) due to an unseen component around the eclipsing binaries explains the tilted sinusoidal changes in their O- C diagrams. The orbital period decrease rates for the systems are estimated as approximately between about 0.7 and 2.5 s per century. It is clearly seen that mass loss effect is more dominant than the expected mass transfer for classical Algols in this study. The minimum mass of the probable third bodies around the eclipsing pairs was calculated to be ⩽0.5 M ⊙ except for UX Leo, in which it was estimated to be approximately 0.9 M ⊙. In order to search for third lights in the light curves of five systems, the V-light curves of the systems were analyzed and their physical and photometric parameters were determined. For UX Leo, a significant third light contribution was determined. We found a very small third light that can be tested using multi-color light curves, for RW Mon, EQ Ori and XZ UMa, while a third light for AX Vul could not be exposed.

  5. THE FIRST PHOTOMETRIC ANALYSES OF THE ALGOL BINARY SYSTEMS GSC 04328-02164 AND GSC 03164-01558

    Energy Technology Data Exchange (ETDEWEB)

    Essam, A.; Hamed, Amal S.; Mohamadien, Ghada F. [National Research Institute of Astronomy and Geophysics, 11421 Helwan, Cairo (Egypt); Youssef, Shahenaz M., E-mail: essam60@yahoo.com [Astronomy Department, Faculty of Science, Cairo University, Cairo (Egypt)

    2016-01-15

    The CCD observations for the eclipsing Algol type binary systems GSC 04328-02164 in wideband BVR{sub c}I{sub c} filters and GSC 03164-01558 in B and I filters have been analyzed using the PHOEBE package (v 0.31a) to determine their orbital and physical parameters. The absolute parameters and evolutionary tracks of the two systems have been determined. The results show that the mass ratio, inclination, distance, and age for the system GSC 04328-02164 are equal to q = 0.674 ± 0.002, i = 75.997 ± 0.022, d = 375.477 ± 4.299 pc, and τ = 26.76 ± 15.65 ∗ 10{sup 8} years, respectively. For the other system, GSC 03164-01558, q = 0.941 ± 0.006, i = 88.0484 ± 0.030, d = 444.651 ± 9.444 pc, and τ = 53.63 ± 9.16 ∗ 10{sup 8} years.

  6. A Spectroscopic Study of the Algol-type Binaries S Equulei and KO Aquilae: Absolute Parameters and Mass Transfer

    CERN Document Server

    Soydugan, F; Soydugan, E; Catalano, S; Demircan, O; Ibanoglu, C

    2007-01-01

    We present and analyze high-resolution optical spectra of the Algol binaries S Equ and KO Aql. New accurate radial velocities for the hotter primary components are obtained. Thanks to the cross-correlation procedure, we were able to measure, for the first time to our knowledge, radial velocities also for the cool secondary components of S Equ and KO Aql. By combining the parameters obtained from the solution of the radial velocity curves with those obtained from the light curve analysis, reliable absolute parameters of the systems have been derived. The rotational velocity of the hotter components of S Equ and KO Aql has been measured and it is found that the gainers of both systems rotate about 30 % faster than synchronously. This is likely due to mass transfer across the Lagrangian L1 point from the cooler to the hotter component. The lower luminosity of the mass-gaining components of these systems compared to normal main-sequence stars of the same mass can be also an effect of the mass transfer. The H-alph...

  7. Multi-site, multi-year monitoring of the oscillating Algol-type eclipsing binary CT Her

    CERN Document Server

    Lampens, P; Kim, S -L; Rodriguez, E; Lopez-Gonzalez, M J; Vidal-Sainz, J; Mkrtichian, D; Koo, J -R; Kang, Y B; Van Cauteren, P; Wils, P; Kraicheva, Z; Dimitrov, D; Southworth, J; Melendo, E Garcia; Forellad, J M Gomez

    2011-01-01

    We present the results of a multi-site photometric campaign carried out in 2004-2008 for the Algol-type eclipsing binary system CT Her, the primary component of which shows Delta Scuti-type oscillations. Our data consist of differential light curves collected in the filters B and V which have been analysed using the method of Wilson-Devinney (PHOEBE). After identification of an adequate binary model and removal of the best-matching light curve solution, we performed a Fourier analysis of the residual B and V light curves to investigate the pulsational behaviour. Up to eight significant frequencies with semi-amplitudes in the range 3 to 1 mmag were detected, all of which surprisingly lie in the frequency range 43.5-53.5 c\\d. This result is independent from the choice of the primary's effective temperature (8200 or 8700 K) since the light curve models for the binary are very similar in both cases. This is the second case of a complex frequency spectrum observed for an accreting Delta Scuti-type star (after Y Ca...

  8. Three-dimensional Doppler Tomogram of Gas Flows in the Algol-Type Binary U Coronae Borealis

    Science.gov (United States)

    Agafonov, Michail; Richards, Mercedes; Sharova, Olga

    2006-12-01

    The reconstruction of three-dimensional (3D) Doppler tomograms based on observational data has been accomplished for the first time. The distribution of the Hα emission intensity I(Vx,Vy,Vz) of the interacting Algol binary system U Coronae Borealis has been restored in 3D velocity space with resolutions of 30 km s-1 in Vx and Vy and 110 km s-1 in Vz. The reconstruction was based on 47 Hα spectra from 1994 by applying the developed radioastronomical approach (RA) to few-projections tomography. The comparison between the previous 2D and our 3D Doppler tomograms shows similarities with the main structural features of the gas flows in the orbital plane. Specifically, the gas stream along the ballistic trajectory and equatorial emission centered on the primary star are displayed on the 3D Doppler tomogram as distinct emission sources. A high-velocity stream (Vz~200 km s-1) with strong emission intensity has also been discovered moving in the direction across the orbital plane of the system.

  9. A comparison between observed Algol-type double stars in the solar neighborhood and evolutionary computations of galactic case A binaries with a B-type primary at birth

    Science.gov (United States)

    Mennekens, N.; Vanbeveren, D.

    2017-03-01

    We first discuss a large set of evolutionary calculations of close binaries with a B-type primary at birth and with a period such that the Roche lobe overflow starts during the core hydrogen burning phase of the primary (intermediate mass and massive case A binaries). The evolution of both components is followed simultaneously allowing us to check for the occurrence of contact binaries. We consider various models to treat a contact system and the influence of these models on the predicted Algol-type system population is investigated. We critically discuss the available observations of Algol-type binaries with a B-type primary at birth. Comparing these observations with the predictions allows us to put constraints on the contact star physics. We find that mass transfer in Algols is most probably not conservative, that contact during this phase does not necessarily lead to a merger, and that angular momentum loss must be moderate.

  10. Photometric Properties for Selected Algol-type Binaries. VIII. The Triple Systems DI Peg and AF Gem Revisited

    Science.gov (United States)

    Yang, Yuan-Gui; Yang, Ying; Li, Shu-Zheng

    2014-06-01

    New extensive photometry for two triple binary stars, DI Peg and AF Gem, was performed from 2012 October to 2013 January, with two small telescopes at Xinglong station (XLs) of NAOC. From new multi-color observations and previously published ones in literature, the photometric models were (re)deduced using the updated Wilson-Devinney code. The results indicated that the low third lights exist in two classic Algol-type binaries, whose fill-out factors for the more massive components are fp = 78.2(± 0.4)% for DI Peg, and fp = 69.0(± 0.3)% for AF Gem, respectively. Through analyzing the O-C curves, the orbital periods for two binaries change in the complicated mode. The period of DI Peg possibly appears to show two light-time orbits, whose modulated periods are P 3 = 54.6(± 0.5) yr and P 4 = 23.0(± 0.6) yr, respectively. The inferred minimum masses for the inner and outer sub-stellar companions are M in = 0.095 M ⊙ and M out = 0.170 M ⊙, respectively. Therefore, DI Peg may be a quadruple star. The orbital period of AF Gem appears to show a continuous period decrease or a cyclic variation; the latter may be preferable. The cyclic oscillation, with a period of 120.3(± 2.5) yr, may be attributed to the light-time effect due to the third body. This kind of additional companion may extract angular momentum from the central system, which may play a key role in the evolution of the binary.

  11. Photometric Properties of Selected Algol-type Binaries. III. AL Geminorum and BM Monocerotis with Possible Light-time Orbits

    Science.gov (United States)

    Yang, Y.-G.; Li, H.-L.; Dai, H.-F.

    2012-01-01

    We present the CCD photometry of two Algol-type binaries, AL Gem and BM Mon, observed from 2008 November to 2011 January. With the updated Wilson-Devinney program, photometric solutions were deduced from their EA-type light curves. The mass ratios and fill-out factors of the primaries are found to be q ph = 0.090(± 0.005) and f 1 = 47.3%(± 0.3%) for AL Gem, and q ph = 0.275(± 0.007) and f 1 = 55.4%(± 0.5%) for BM Mon, respectively. By analyzing the O-C curves, we discovered that the periods of AL Gem and BM Mon change in a quasi-sinusoidal mode, which may possibly result from the light-time effect via the presence of a third body. Periods, amplitudes, and eccentricities of light-time orbits are 78.83(± 1.17) yr, 0fd0204(±0fd0007), and 0.28(± 0.02) for AL Gem and 97.78(± 2.67) yr, 0fd0175(±0fd0006), and 0.29(± 0.02) for BM Mon, respectively. Assumed to be in a coplanar orbit with the binary, the masses of the third bodies would be 0.29 M ⊙ for AL Gem and 0.26 M ⊙ for BM Mon. This kind of additional companion can extract angular momentum from the close binary orbit, and such processes may play an important role in multiple star evolution.

  12. Lunar-based Ultraviolet Telescope study of the well-known Algol-type binary TW Dra

    Science.gov (United States)

    Liao, Wen-Ping; Qian, Sheng-Bang; Zejda, Miloslav; Zhu, Li-Ying; Li, Lin-Jia

    2016-06-01

    By using the Lunar-based Ultraviolet Telescope (LUT) from 2014 December 2 to December 4, the first near-UV light curve of the well-known Algol-type binary TW Dra is reported, which is analyzed with the 2013 version of the W-D code. Our solutions confirmed that TW Dra is a semi-detached binary system where the secondary component fills its Roche lobe. The mass ratio and a high inclination are obtained (q = 0.47, i = 86.68°). Based on 589 available data spanning more than one century, the complex period changes are studied. Secular increase and three cyclical changes are found in the corresponding orbital period analysis. The secular increase changes reveal mass transfer from the secondary component to the primary one at a rate of 6.8 × 10-7 M ⊙ yr-1. One large cyclical change of 116.04 yr may be caused by disturbance of visual component ADS 9706B orbiting TW Dra (ADS 9706A), while the other two cyclical changes with shorter periods of 22.47 and 37.27 yr can be explained as the result of two circumbinary companions that are orbiting around TW Dra, where the two companions are in simple 3 : 5 orbit-rotation resonances. TW Dra itself is a basic binary in a possible sextuple system with the configuration (1 + 1) + (1 + 1) + (1 + 1), which further suggests that multiplicity may be a fairly common phenomenon in close binary systems.

  13. First analysis of eight Algol-type binaries: EI Aur, XY Dra, BP Dra, DD Her, VX Lac, WX Lib, RZ Lyn, and TY Tri

    CERN Document Server

    Zasche, P

    2015-01-01

    The available photometry from the online databases were used for the first light curve analysis of eight eclipsing binary systems EI Aur, XY Dra, BP Dra, DD Her, VX Lac, WX Lib, RZ Lyn, and TY Tri. All these stars are of Algol-type, having the detached components and the orbital periods from 0.92 to 6.8 days. For the systems EI Aur and BP Dra the large amount of the third light was detected during the light curve solution. Moreover, 468 new times of minima for these binaries were derived, trying to identify the period variations. For the systems XY Dra and VX Lac the third bodies were detected with the periods 17.7, and 49.3 years, respectively.

  14. A comparison between observed Algol-type double stars in the Solar neighborhood and evolutionary computations of galactic case A binaries with a B-type primary at birth

    CERN Document Server

    Mennekens, N

    2016-01-01

    We first discuss a large set of evolutionary calculations of close binaries with a B-type primary at birth and with a period such that the Roche lobe overflow starts during the core hydrogen burning phase of the primary (intermediate mass and massive case A binaries). The evolution of both components is followed simultaneously allowing us to check for the occurrence of contact binaries. We consider various models to treat a contact system and the influence of these models on the predicted Algol-type system population is investigated. We critically discuss the available observations of Algol-type binaries with a B-type primary at birth. Comparing these observations with the predictions allows us to put constraints on the contact star physics.

  15. The chemical composition of algol systems. III - Beta Lyrae-nucleosynthesis revealed

    Science.gov (United States)

    Balachandran, S.; Lambert, D. L.; Tomkin, J.; Parthasarathy, M.

    1986-04-01

    The B8 primary of the eclipsing binary star Beta Lyr is subjected to high S/N ratio Reticon observations of the visible and near-IR lines of He, C, N, O, Ne, and Fe, in order to determine their abundances. N is noted to be extremely overabundant (20 times more so than in the sun); C and O are very overabundant relative to N. The resulting C/N and O/N ratios of respectively 5 and 8 are sufficiently close to the equilibrium ratios of the CNO cycle as to leave little doubt that the material has been fully processed by the CNO cycle. The spectroscopic evidence found for He enrichment and extreme CNO cycling confirms the major compositional changes demanded by the theory of nuclear burning, thereby supporting current understanding of Beta Lyr.

  16. Photometric Properties for Selected Algol-type Binaries. II. AO Serpentis and V338 Herculis

    Science.gov (United States)

    Yang, Y.-G.; Hu, S.-M.; Guo, D.-F.; Wei, J.-Y.; Dai, H.-F.

    2010-04-01

    We present the first multiband photometry for the semidetached eclipsing binary AO Serpentis, observed on seven nights between 2009 April and July at the Weihai Observatory of Shandong University. By using the 2003 version of the Wilson-Devinney code, the photometric solutions of AO Ser and a similar object V338 Her were (re)deduced. The spectral types and orbital periods are A2 and P = 0.8793 days for AO Ser, F1V and P = 1.3057 days for V338 Her. The results reveal that two binaries are low mass ratio systems, whose secondary components fill their Roche lobes. The fill-out factors of the primary components are f = 58.6% for AO Ser and f = 54.2% for V338 Her, respectively. From the O - C curves of AO Ser and V338 Her, it is discovered that secular period changes with cyclic variations exist. The periods and semiamplitudes are 17.32(±0.01) yr and 0.0051(±0.0001) days for AO Ser, 29.07(±0.04) yr and 0.0116(±0.0015) days for V338 Her, respectively. This kind of cyclic oscillation may be attributed to either the light-time effect via an assumed third body or perhaps cyclic magnetic activity on the secondary component. For AO Ser, the long-term period decreases at a rate of dP/dt = -5.35(±0.03) × 10-7 days yr-1, which may be caused by mass and angular momentum loss from the system. Considering the period decreasing, the fill-out factor of the primary for AO Ser will increase and it will finally fill its Roche lobe. Meanwhile, the secular period increase rate for V338 Her is dP/dt = +1.44(±0.24) × 10-7 days yr-1, indicating that mass transfers from the less massive component to the more massive component. This will also cause the fill-out factor of the primary to increase. When the primaries fill their Roche lobes, AO Ser and V338 Her may evolve into contact stars, as predicted by the theory of thermal relaxation oscillations.

  17. Binarity and Pulsation in Algol-type Binary System SX Draconis

    Science.gov (United States)

    Soydugan, E.; Kaçar, Y.

    2013-04-01

    Photometric observations of SX Dra were carried out to determine the properties of the components and pulsational characteristics of the more massive pulsational component. Physical parameters of the component stars were obtained by modeling B and V light curves using the Wilson-Devinney code. Results indicate that SX Dra is a semi-detached system with the secondary component filling its Roche lobe. The O-C data showed parabolic and sinusoidal variation. Cyclic variation in the O-C diagram could be the result of the possible magnetic activity of the secondary component instead of the third body. The secular increase in the orbital period of the system can be interpreted as being the result of mass transfer from the secondary component to the primary one at a rate of 2.1 × 10-7 M ⊙ yr-1. Results of a time-series analysis performed after removing binary effects indicated that the hot component shows δ Scuti light variations with pulsational periods of 63 and 73 minutes. Spherical harmonic degrees (l) were determined to be 3 for the first frequency and 1-2 for the second frequency.

  18. Orbital period changes and possible stellar wind mass loss in the algol-type binary system AT Pegasi

    Directory of Open Access Journals (Sweden)

    Magdy A. Hanna

    2012-12-01

    Full Text Available An analysis of the measurements of mid-eclipse times of AT Peg has been presented. It indicates a period decrease rate of dP/dt = −4.2 × 10−7 d/yr, which can be interpreted in terms of mass loss from the system via stellar wind with a rate between (1 and 2 × 10−8 Mʘ/yr. The O–C diagram shows a growing sine wave covering two different cycles of 13 yr and 31.9 yr with amplitudes equal to 0.026 and 0.032 day, respectively. These unequal durations of the cycles may be explained by magnetic activity cycling variations due to star spots. The obtained characteristics of the second cycle are consistent with similar systems when applying Applegate’s mechanism.

  19. ALGOL-M. An Implementation of a High-level Block Structured Language for a Microprocessor-based Computer System

    Science.gov (United States)

    1977-09-01

    lag’ Ta meg It signO and algal then dot eIgu2 z:positive; ret urni end: sIgn2 z’ negativel If not signO and not signl thL-vi do: 56? iag true; re...turn: end: If signO then call complimsnet, 1). else cult compliment(@); end checiklulgnt add: procedure: call check~sign: 091l addfrg(.rl,.r2)t call

  20. On the Question of the Behavior of O-C Residuals of the Active Algol-Like Binary RZ Cassiopeiae

    CERN Document Server

    Golovin, A; Golovin, Alex; Pavlenko, Elena

    2005-01-01

    We present an analysis of the RZ Cassiopeia O-C diagram for a 30-year period, based on data published by the AAVSO. The new parabolic light-elements are determined and P-dot was estimated. This enabled us to establish the value of M-dot, the rate of the mass transfer between components of this eclipsing binary. Deviations from the parabola in the RZ Cas O-C diagram have a wavelike trend. The pulsation of the primary component influences the scatter of O-C points, as well as it influences the shape of the eclipse. Some physical points on such O-C behavior are presented.

  1. J Is for JavaScript: A Direct-Style Correspondence between Algol-Like Languages and JavaScript Using First-Class Continuations

    DEFF Research Database (Denmark)

    Danvy, Olivier; Shan, Chung-chieh; Zerny, Ian Steven

    2009-01-01

    the same block structure and binding structure as in the source program, à la Abdali. The target code uses a control operator in direct style, à la Landin. In fact, the control operator used is almost Landin’s J—hence our title. Our translation thus complements a continuation-passing translation à la...

  2. Annual review in automatic programming

    CERN Document Server

    Goodman, Richard

    2014-01-01

    Annual Review in Automatic Programming, Volume 4 is a collection of papers that deals with the GIER ALGOL compiler, a parameterized compiler based on mechanical linguistics, and the JOVIAL language. A couple of papers describes a commercial use of stacks, an IBM system, and what an ideal computer program support system should be. One paper reviews the system of compilation, the development of a more advanced language, programming techniques, machine independence, and program transfer to other machines. Another paper describes the ALGOL 60 system for the GIER machine including running ALGOL pro

  3. A Garbage Collector for a Large Distributed Address Space,

    Science.gov (United States)

    1985-06-01

    Memory 5 The Garbage Collector 6 Practical Implementation 7 Conclusions 8 Acknowledgements 9 Reference Appendix A. Algorithm in Pidgin Algol e’ * * S...lowest level, but also contributes to the garbage collection of the higher level areas above it. The algorithm is given in pidgin Algol in Appendix A...NJECESSARILY AV.-tLAfq F 10 MFMF:rRS 6’ INE PUBLIC OR TUOW-VMERCIAL ORG ,N’ ,ONS 13 APPENDIX A. Algorithm In Pidgin Algol. TYPE COLOUR - (whlte,grey

  4. Sorting by Recursive Partitioning,

    Science.gov (United States)

    1983-12-01

    asymptotic time-complexity. This paper has the following main parts: First, a Pidgin -Algol version of the algorithm is presented and we discuss the main...those sorted subsets e) end "UsingBin*; end "AdaptSorting. 4 "Figure 1: A condensed Pidgin -Algol version of Adaptsort eiFor some conditions that we will...algorithm which have to be completed in either linear or constant times (these required critical times appear as comments in the Pidgin -Algol version

  5. Distributed Minimum Hop Algorithms

    Science.gov (United States)

    1982-01-01

    acknowledgement), node d starts iteration i+1, and otherwise the algorithm terminates. A detailed description of the algorithm is given in pidgin algol...precise behavior of the algorithm under these circumstances is described by the pidgin algol program in the appendix which is executed by each node. The...l) < N!(2) for each neighbor j, and thus by induction,J -1 N!(2-1) < n-i + (Z-1) + N!(Z-1), completing the proof. Algorithm Dl in Pidgin Algol It is

  6. Average Case Analysis of an Adjacency Map Searching Technique.

    Science.gov (United States)

    1981-12-01

    next section (see Figure 2.2 (c)). A pidgin algol program for procedure SEARCHTREE is given in Table 1. Q Q 1 1 Q29 U, Z are queues; s Q and Q s denote...rectangle to which they belong. In a second scan, a list Pi of sorted points is easily built for I° Table 1. A pidgin algol program for procedure

  7. Annual review in automatic programming

    CERN Document Server

    Goodman, Richard

    2014-01-01

    Annual Review in Automatic Programming focuses on the techniques of automatic programming used with digital computers. Topics covered range from the design of machine-independent programming languages to the use of recursive procedures in ALGOL 60. A multi-pass translation scheme for ALGOL 60 is described, along with some commercial source languages. The structure and use of the syntax-directed compiler is also considered.Comprised of 12 chapters, this volume begins with a discussion on the basic ideas involved in the description of a computing process as a program for a computer, expressed in

  8. John Goodricke, Edward Pigott, and Their Study of Variable Stars

    CERN Document Server

    French, L M

    2012-01-01

    John Goodricke and Edward Pigott, working in York, England, between 1781 and 1786, determined the periods of variation of eclipsing binaries such as Algol and Beta Lyrae and speculated that the eclipses of Algol might be caused by a "dark body," perhaps even a planet. They also determined the periods of variation of the first two known Cepheid variables, the stars whose period-luminosity relation today enables astronomers to determine distances to distant galaxies. Goodricke holds special interest because he was completely deaf and because he died at the age of 21. The lives and work of these two astronomers are described.

  9. Searching for Variable Stars in and around Open Clusters

    Institute of Scientific and Technical Information of China (English)

    2002-01-01

    We present a snapshot of our recent results of a variable star survey in1 degree fields around three open clusters: NGC 188, NGC 7789 and M67. A totalnumber of 39 variable stars are newly discovered, including 22 W UMa stars, 10EA (Algol) type binaries, one RR-lyr and one RRd pulsator, and five unclassifiedvariables.

  10. Language-Based Security for Malicious Mobile Code

    Science.gov (United States)

    2007-09-30

    Algol), and the Berkeley SDS-940 system employed object-code rewriting as part of its system pro- filer. More recently, the SPIN [5], Vino [52, 47], and...1993. [52] E. Yasuhiro, J. Gwertzman, M. Seltzer, C. Small, Keith A. Smith, and D. Tang. VINO : The 1994 fall harvest. Technical Report TR-34-94

  11. [Computer programming for radiocardiography and radiocyclography].

    Science.gov (United States)

    Khorvat, M; Sabo, D; Tomor, B; Almashi, L; Debretsi, T; Ludvig, K

    1977-09-01

    Digital radiocardiography with linear programming, on the ALGOL language, by means of an ODRA-1204 computer is described. Determination of cardiac dynamical parameters of patients in rest and under load was carried out. Radioisotopic methods were combined with conventional cardiologic examinations, particularly the microcatheterization.

  12. Real-World Experimentation Comparing Time-Sharing and Batch Processing in Teaching Computer Science,

    Science.gov (United States)

    effectiveness of time-sharing and batch processing in teaching computer science . The experimental design was centered on direct, ’real world’ comparison...ALGOL). The experimental sample involved all introductory computer science courses with a total population of 415 cadets. The results generally

  13. Recursive Programming: A Clarification

    NARCIS (Netherlands)

    Hove d'Ertsenryck, G.M.C. van den

    2012-01-01

    We show that the block concept, as it was introduced in ALGOL 60, and two of the three main techniques introduced by E. W. Dijkstra in his seminal article Recursive Programming to implement it, the so-called "static links" and "display", have been partly misunderstood. These misunderstandings may ha

  14. Orbit and spin evolution of synchronous binary stars on the main sequence

    Institute of Scientific and Technical Information of China (English)

    Lin-Sen Li

    2012-01-01

    A set of synchronous equations are derived from a set of non-synchronous equations.The analytical solutions are given by solving the set of differential equations.The results of the evolutionary trend of the spin-orbit interaction are that the semi-major axis gradually shrinks with time; the orbital eccentricity gradually decreases with time until orbital circularization occurs; the orbital period gradually shortens with time and the rotational angular velocity of the primary component gradually speeds up with time before the orbit achieves circularization.The theoretical results are applied to evolution of the orbit and spin of synchronous binary stars Algol A and B that are on the main sequence.The circularization time,lifetime and the evolutionary numerical solutions of orbit and spin when circularization time occurs are estimated for Algol A and B.

  15. Applications of Doppler Tomography in 2D and 3D

    Science.gov (United States)

    Richards, M.; Budaj, J.; Agafonov, M.; Sharova, O.

    2010-12-01

    Over the past few years, the applications of Doppler tomography have been extended beyond the usual calculation of 2D velocity images of circumstellar gas flows. This technique has now been used with the new Shellspec spectrum synthesis code to demonstrate the effective modeling of the accretion disk and gas stream in the TT Hya Algol binary. The 2D tomography procedure projects all sources of emission onto a single central (Vx, Vy) velocity plane even though the gas is expected to flow beyond that plane. So, new 3D velocity images were derived with the Radioastronomical Approach method by assuming a grid of Vz values transverse to the central 2D plane. The 3D approach has been applied to the U CrB and RS Vul Algol-type binaries to reveal substantial flow structures beyond the central velocity plane.

  16. Variability survey in the CoRoT SRa01 field: Implications of eclipsing binary distribution on cluster formation in NGC 2264

    CERN Document Server

    Klagyivik, P; Pasternacki, T; Fruth, T; Erikson, A; Cabrera, J; Chini, R; Eigmüller, P; Kabath, P; Kirste, S; Lemke, R; Murphy, M; Rauer, H; Titz-Weider, R

    2013-01-01

    Time-series photometry of the CoRoT field SRa01 was carried out with the Berlin Exoplanet Search Telescope II (BEST II) in 2008/2009. A total of 1,161 variable stars were detected, of which 241 were previously known and 920 are newly found. Several new, variable young stellar objects have been discovered. The study of the spatial distribution of eclipsing binaries revealed the higher relative frequency of Algols toward the center of the young open cluster NGC 2264. In general Algol frequency obeys an isotropic distribution of their angular momentum vectors, except inside the cluster, where a specific orientation of the inclinations is the case. We suggest that we see the orbital plane of the binaries almost edge-on.

  17. VARIABILITY SURVEY IN THE CoRoT SRa01 FIELD: IMPLICATIONS OF ECLIPSING BINARY DISTRIBUTION ON CLUSTER FORMATION IN NGC 2264

    Energy Technology Data Exchange (ETDEWEB)

    Klagyivik, P. [Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, H-1121 Budapest XII, Konkoly Thege ut 15-17. (Hungary); Csizmadia, Sz.; Pasternacki, T.; Fruth, T.; Erikson, A.; Cabrera, J.; Eigmueller, P.; Kirste, S.; Rauer, H.; Titz-Weider, R. [Institut fuer Planetenforschung, Deutsches Zentrum fuer Luft- und Raumfahrt, Rutherfordstrasse 2, D-12489 Berlin (Germany); Chini, R.; Lemke, R. [Astronomisches Institut, Ruhr-Universitaet Bochum, D-44780 Bochum (Germany); Kabath, P. [European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago (Chile); Murphy, M. [Depto. Fisica, Universidad Catolica del Norte, PO 1280, Antofagasta (Chile)

    2013-08-10

    Time-series photometry of the CoRoT field SRa01 was carried out with the Berlin Exoplanet Search Telescope II in 2008/2009. A total of 1161 variable stars were detected, of which 241 were previously known and 920 are newly found. Several new, variable young stellar objects have been discovered. The study of the spatial distribution of eclipsing binaries revealed the higher relative frequency of Algols toward the center of the young open cluster NGC 2264. In general Algol frequency obeys an isotropic distribution of their angular momentum vectors, except inside the cluster, where a specific orientation of the inclinations is the case. We suggest that we see the orbital plane of the binaries almost edge-on.

  18. Thunks and the λ-calculus

    DEFF Research Database (Denmark)

    Hatcliff, John; Danvy, Olivier

    1997-01-01

    Thirty-five years ago, thunks were used to simulate call-by-name under call-by-value in Algol 60. Twenty years ago, Plotkin presented continuation-based simulations of call-by-name under call-by-value and vice versa in the λ-calculus. We connect all three of these classical simulations by factori......Thirty-five years ago, thunks were used to simulate call-by-name under call-by-value in Algol 60. Twenty years ago, Plotkin presented continuation-based simulations of call-by-name under call-by-value and vice versa in the λ-calculus. We connect all three of these classical simulations...

  19. Thunks and the λ-calculus

    DEFF Research Database (Denmark)

    Hatcliff, John; Danvy, Olivier

    1996-01-01

    Thirty-five years ago, thunks were used to simulate call-by-name under call-by-value in Algol 60. Twenty years ago, Plotkin presented continuation-based simulations of call-by-name under call-by-value and vice versa in the λ-calculus. We connect all three of these classical simulations by factori......Thirty-five years ago, thunks were used to simulate call-by-name under call-by-value in Algol 60. Twenty years ago, Plotkin presented continuation-based simulations of call-by-name under call-by-value and vice versa in the λ-calculus. We connect all three of these classical simulations...

  20. Algorithms over partially ordered sets

    DEFF Research Database (Denmark)

    Baer, Robert M.; Østerby, Ole

    1969-01-01

    in partially ordered sets, answer the combinatorial question of how many maximal chains might exist in a partially ordered set withn elements, and we give an algorithm for enumerating all maximal chains. We give (in § 3) algorithms which decide whether a partially ordered set is a (lower or upper) semi......-lattice, and whether a lattice has distributive, modular, and Boolean properties. Finally (in § 4) we give Algol realizations of the various algorithms....

  1. Annual review in automatic programming

    CERN Document Server

    Halpern, Mark I; Bolliet, Louis

    2014-01-01

    Computer Science and Technology and their Application is an eight-chapter book that first presents a tutorial on database organization. Subsequent chapters describe the general concepts of Simula 67 programming language; incremental compilation and conversational interpretation; dynamic syntax; the ALGOL 68. Other chapters discuss the general purpose conversational system for graphical programming and automatic theorem proving based on resolution. A survey of extensible programming language is also shown.

  2. Program verification using symbolic game semantics

    OpenAIRE

    Dimovski, Aleksandar

    2014-01-01

    We introduce a new symbolic representation of algorithmic game semantics, and show how it can be applied for efficient verification of open (incomplete) programs. The focus is on an Algol-like programming language which contains the core ingredients of imperative and functional languages, especially on its second-order recursion-free fragment with infinite data types. We revisit the regular-language representation of game semantics of this language fragment.By using symbolic values instead of...

  3. Theory and practice of compilation

    CERN Document Server

    Langmaack, H

    1972-01-01

    Compilation is the translation of high level language programs into machine code. Correct translation can only be achieved if syntax and semantics of programming languages are clearly defined and strictly obeyed by compiler constructors. The author presents a simple extendable scheme for syntax and semantics to be defined rigorously. This scheme fits many programming languages, especially ALGOL-like ones. The author considers statements and programs to be notations of state transformations; in special cases storage state transformations. (5 refs).

  4. Computerized calculation of material balances in carbonization

    Energy Technology Data Exchange (ETDEWEB)

    Chistyakov, A.M.

    1980-09-01

    Charge formulations and carbonisation schedules are described by empirical formulae used to calculate the yield of coking products. An algorithm is proposed for calculating the material balance, and associated computer program. The program can be written in conventional languages, e.g. Fortran, Algol etc. The information obtained can be used for on-line assessment of the effects of charge composition and properties on the coke and by-products yields, as well as the effects of the carbonisation conditions.

  5. NZ Ser: the results of the analysis of the 25 years photometric activity

    Science.gov (United States)

    Barsunova, O.; Mel'nikov, S.; Grinin, V.; Katysheva, N.; Shugarov, S.

    2014-03-01

    We present the analysis of the long-term photometric variability of NZ Ser. The object shows both large-scale cyclic variability and low-amplitude Algol-like, fading typical for UX Ori stars. The variations of the stellar brightness are accompanied by variations of the B-V and V-R colors: when the brightness decreases, B-V decreases, while V-R increases.

  6. Defense Information Systems Agency Technical Integration Support (DISA- TIS). MUMPS Study.

    Science.gov (United States)

    1993-01-01

    programming language; it includes facilities for both high- and low-level programming . C supports low-level hardware control and bit manipulation in addition...purposes. Sup- porting structured programming C 1974 D. Ritchie ALGOL 68 Systems programming (Bell Labs) BCPL Ada 1979 J. lchbiah eta.. Pascal, General...requirements and has high de facto usage for scientific and mathematical programming . C also provides support for efficient array and matrix calculations

  7. Cost Benefit Assessment of Candidate Decision Aids for Naval Air ASW.

    Science.gov (United States)

    1981-09-01

    this extended HOPROC, which is termed " pidgin -HOPROC" after the " pidgin -ALGOL" invented by Aho, Hopcroft, and Ullman (1974) for the analysis of computer...algorithms. From this third step two sequences of pidgin -HOPROC statements for each scenario evolution are produced -- one for the current (unaided...evolution on the scenario tree. Thus in the fourth step, the pidgin -HOPROC sequences are combined with the *A more thorough discussion of the advantages

  8. A new photometric and spectroscopic study of the eclipsing binaries CC Her and CM Lac: Physical parameters and evolutionary status

    CERN Document Server

    Liakos, Alexios

    2014-01-01

    New complete light and radial velocities curves were obtained for the eclipsing binaries CC Her and CM Lac. The data are analysed with modern techniques in order to derive the physical parameters of the systems and study their present evolutionary status. We found that CC Her is a classical Algol type binary, while CM Lac is a detached system with two Main Sequence stars in asynchronous orbit.

  9. Statistically Optimal Determination of the Phenomenological Parameters of the Phase Light Curves of Eclipsing Binaries. The Structure of the Test Function

    CERN Document Server

    Tkachenko, Mariia G

    2016-01-01

    The dependence of the test function on the phenomenological parameters used in the "NAV" ("New Algol Variable") algorithm (Andronov, 2012Ap.....55..536A) is studied. Due to a presence of local minima, the method of minimization contains two steps: the "brute force" minimization at a grid in the 4D parameter space, and further iterations using the differential corrections. This method represents an effective approximation of the light curve using the special pattern (shape) separately for the primary and secondary minima. The application of the method to concrete stars is briefly reviewed.

  10. Programming language structures

    CERN Document Server

    Organick, Elliott Irving; Plummer, Robert P

    1978-01-01

    Programming Language Structures deals with the structures of programming languages and introduces the reader to five important programming languages: Algol, Fortran, Lisp, Snobol, and Pascal. The fundamental similarities and differences among these languages are discussed. A unifying framework is constructed that can be used to study the structure of other languages, such as Cobol, PL/I, and APL. Several of the tools and methodologies needed to construct large programs are also considered.Comprised of 10 chapters, this book begins with a summary of the relevant concepts and principles about al

  11. Contribución al conocimiento del género "Oedogonium" (Oedogoniales, Chlorophyta) en España II

    OpenAIRE

    Cambra Sánchez, Jaume

    1992-01-01

    Se presentan los resultados de un estudio florístico sobre el género Oedogonium en España. En total se han estudiado 13 localidades en las que se han identificado 14 táxones, entre los cuales cabe destacar la presencia de Oedogonium khannae f. minus, Oedogonium lopesianum y Oedogonium pratense, que constituyen tres nuevas citas para la flora algológica española. Se describen la mayoría de los táxones, así como se realizan comentarios sobre su distribución y posición taxonómica.

  12. Binary stars: Mass transfer and chemical composition

    Science.gov (United States)

    Lambert, D. L.

    1982-01-01

    It is noted that mass exchange (and mass loss) within a binary system should produce observable changes in the surface chemical composition of both the mass losing and mass gaining stars as a stellar interior exposed to nucleosyntheses is uncovered. Three topics relating mass exchange and/or mass loss to nucleosynthesis are sketched: the chemical composition of Algol systems; the accretion disk of a cataclysmic variable fed by mass from a dwarf secondary star; and the hypothesis that classical Ba II giants result from mass transfer from a more evolved companion now present as a white dwarf.

  13. Modeling Gyrosynchrotron Coronae of Radio-Loud Stars

    Science.gov (United States)

    Peterson, William M.

    2015-01-01

    Fast gyrosynchrotron codes are used to model the emission in close, active binary star systems. Multiple magnetic field topologies, plasma densities, and scale heights for the emitting plasma are tested for in an attempt to duplicate the emission characteristics detected using high-resolution VLBI imaging of the close active binaries UX Arietis and Algol. Also included are effects of occlusion by the companion star. It is found that a co-orbiting coronal loop oriented toward the companion star with its feet anchored on the poles of the active star is consistent with the observed emission from these two radio-loud stars.

  14. The first light-curve analysis of eclipsing binaries observed by the INTEGRAL/OMC

    CERN Document Server

    Zasche, P

    2008-01-01

    Three Algol-type binaries in Cygnus constellation were selected for an analysis from a huge database of observations made by the INTEGRAL/OMC camera. These data were processed and analyzed, resulting in a first light-curve study of these neglected eclipsing binaries. The temperatures of the primary components range from 9500 K to 10500 K and the inclinations are circa 73deg (for PV Cyg and V1011 Cyg), while almost 90deg for V822 Cyg. All of them seem to be main-sequence stars, well within their critical Roche lobes. Nevertheless, further detailed analyses are still needed.

  15. Binaires semi-détachées : taxonomie

    Science.gov (United States)

    Hameury, Jean-Marie

    2001-01-01

    We discuss here compact binaries in which the orbital separation is small enough that mass is transferred from one star to the other. These systems are classified according to the nature of the primary: algols for ordinary stars, cataclysmic variables for white dwarfs, and X-ray binaries for black holes and neutron stars. These classes are often studied separately, even though the same physical processes occur in all objects; a global approach is most useful for understanding these objects and the physical processes. On discutera ici des binaires serrées dans lesquelles la séparation est suffisamment faible pour qu'il y ait échange de matière entre les deux étoiles. La classification de ces systèmes est liée à la nature de l'étoile accrétante: algols pour la séquence principale, variables cataclysmiques pour les naines blanches, et binaires X pour les étoiles à neutrons ou les trous noirs. Ces classes sont souvent étudiées de façon séparée, mais elles révèlent des processus physiques communs; la compréhension des objets et de la physique sous-jacente bénéficie d'une approche globale.

  16. X-ray spectroscopy of late-type stars. [HEAO 2 observations

    Science.gov (United States)

    Swank, J. H.; White, N. E.

    1980-01-01

    The solid state spectrometer on the Einstein Observatory determined .4 - 4.5 keV spectra for Capella, Algol and 6 RS CVn binaries. All show evidence for a bimodal distribution of emission measure with temperature with one component approximately 7 million degrees and one approximately 40 million degrees. The spread in values of both luminosity and emission measure is 10 for the low temperature component and approximately 500 for the high temperature component. Line emission due to Fe can be identified in most of them and abundances of Si, S and Fe are consistent with approximately solar values in all cases. Estimates indicate dimensions of the emitting regions are on the order of the stellar size and the binary separation for the low and high temperature components, respectively, unless the pressures are high. Variations in the flux were observed, mostly in the hard component for the RS CVn binaries, in the soft component for Capella. A flare was observed during primary eclipse of Algol. The possibility is discussed that the other variations could all be due to intrinsic variability with a time scale of hours-days rather than eclipse or modulation with photometric phase.

  17. Phemenological Modelling of a Group of Eclipsing Binary Stars

    CERN Document Server

    Andronov, Ivan L; Chinarova, Lidia L

    2015-01-01

    Phenomenological modeling of variable stars allows determination of a set of the parameters, which are needed for classification in the "General Catalogue of Variable Stars" and similar catalogs. We apply a recent method NAV ("New Algol Variable") to eclipsing binary stars of different types. Although all periodic functions may be represented as Fourier series with an infinite number of coefficients, this is impossible for a finite number of the observations. Thus one may use a restricted Fourier series, i.e. a trigonometric polynomial (TP) of order s either for fitting the light curve, or to make a periodogram analysis. However, the number of parameters needed drastically increases with decreasing width of minimum. In the NAV algorithm, the special shape of minimum is used, so the number of parameters is limited to 10 (if the period and initial epoch are fixed) or 12 (not fixed). We illustrate the NAV method by application to a recently discovered Algol-type eclipsing variable 2MASS J11080308-6145589 (in the...

  18. Phenomenological Modelling of a Group of Eclipsing Binary Stars

    Science.gov (United States)

    Andronov, Ivan L.; Tkachenko, Mariia G.; Chinarova, Lidia L.

    2016-03-01

    Phenomenological modeling of variable stars allows determination of a set of the parameters, which are needed for classification in the "General Catalogue of Variable Stars" and similar catalogs. We apply a recent method NAV ("New Algol Variable") to eclipsing binary stars of different types. Although all periodic functions may be represented as Fourier series with an infinite number of coefficients, this is impossible for a finite number of the observations. Thus one may use a restricted Fourier series, i.e. a trigonometric polynomial (TP) of order s either for fitting the light curve, or to make a periodogram analysis. However, the number of parameters needed drastically increases with decreasing width of minimum. In the NAV algorithm, the special shape of minimum is used, so the number of parameters is limited to 10 (if the period and initial epoch are fixed) or 12 (not fixed). We illustrate the NAV method by application to a recently discovered Algol-type eclipsing variable 2MASS J11080308-6145589 (in the field of previously known variable star RS Car) and compare results to that obtained using the TP fits. For this system, the statistically optimal number of parameters is 44, but the fit is still worse than that of the NAV fit. Application to the system GSC 3692-00624 argues that the NAV fit is better than the TP one even for the case of EW-type stars with much wider eclipses. Model parameters are listed.

  19. Parallel computations in linear algebra. II

    Energy Technology Data Exchange (ETDEWEB)

    Faddeeva, V.N.; Faddeev, D.K.

    1982-05-01

    For pt.I, see Kibernetika, vol.13, no.6, p.28 (1977). Considerable effort was devoted in the surveyed period to automatic decomposition of sequential algorithms, or rather of procedures or subprograms written in the algorithmic languages ALGOL or FORTRAN. The authors do not consider this body of research, they only note that, on the one hand, the available linear algebra subprograms included in Eispack provide convenient objects for testing various approaches to automatic construction of parallel programs and, on the other, an important state in this activity is the development of methods for fast and efficient solution of linear recurrences, which reduce to solving systems of linear equations with band-triangular matrix (in particular, of sufficiently small width). This article reflects the penetration of the parallelism ideas into the computational methods of linear algebra in recent years. 74 references.

  20. NSV 1907 - A new eclipsing, nova-like cataclysmic variable

    CERN Document Server

    Hümmerich, Stefan; Hambsch, Franz-Josef; Dubois, Franky; Ashley, Richard; Gänsicke, Boris T; Vanaverbeke, Siegfried; Bernhard, Klaus; Wils, Patrick

    2016-01-01

    NSV 1907, formerly listed as an irregular variable in variability catalogues, was classified as an Algol-type eclipsing binary in the Catalina Surveys Periodic Variable Star Catalogue. We have identified NSV 1907 as an ultraviolet (UV) bright source using measurements from the GALEX space telescope and detected obvious out-of-eclipse variability in archival photometric data from the Catalina Sky Survey, which instigated a closer examination of the object. A spectrum and extensive multicolour photometric observations were acquired, from which we deduce that NSV 1907 is a deeply eclipsing, nova-like cataclysmic variable. Apart from the orbital variations (deep eclipses with a period of P ~ 6.63 hours), changes in mean brightness and irregular short-term variability (flickering) were observed. The presence of a secondary minimum at phase phi ~ 0.5 was established, which indicates a significant contribution of the companion star to the optical flux of the system. We find possible evidence for sinusoidal variation...

  1. Comparative Analysis of Phenomenological Approximations of the Light Curves of Eclipsing Binary Stars with Additional Parameters

    CERN Document Server

    Andronov, Ivan L; Chinarova, Lidia

    2016-01-01

    A comparative analysis of the special shapes (patterns, profiles) of the eclipses applied for the phenomenological modeling of the light curves of eclipsing binary stars is conducted. Families of functions are considered, generalizing local approximations (Andronov, 2010, 2012) and the functions theoretically unlimited in a width, based on a Gaussian (Mikulasek, 2015). For an analysis, the light curve of the star V0882 Car = 2MASS J11080308 - 6145589 of the classic Algol - subtype (\\beta Persei) is used. By analyzing dozens of modified functions with additional parameters, it was chosen the 14 best ones according to the criterion of the least sum of squares of deviations. The best are the functions with an additional parameter, describing profiles, which are limited in phase.

  2. VizieR Online Data Catalog: Period of HD 19356 recorded in the Cairo Calendar? (Jetsu+, 2013)

    Science.gov (United States)

    Jetsu, L.; Porceddu, S.; Lyytinen, J.; Kajatkari, P.; Lehtinen, J.; Markkanen, T.; Toivari-Viitala, J.

    2016-08-01

    Ancient Egyptian Scribes (AES) wrote Calendars of Lucky and Unlucky Days that assigned good and bad prognoses for the days of the year. These prognoses were based on mythological and astronomical events considered influential for everyday life. The best preserved calendar is the Cairo Calendar (CC) in papyrus Cairo 86637 dated to 1271-1163B.C. Here, we concentrate on statistics, astrophysics, and astronomy. We show that n~200 good prognoses would induce PMoon and PAlgol in CC, even if the remaining n~700 good and bad prognoses had aperiodic origins. The connections between Algol and AES are discussed in detail in S. Porceddu et al. (2013, in preparation, Paper III), where we date CC to 1224 B.C. (2 data files).

  3. Flowcharting with D-charts

    Science.gov (United States)

    Meyer, D.

    1985-01-01

    A D-Chart is a style of flowchart using control symbols highly appropriate to modern structured programming languages. The intent of a D-Chart is to provide a clear and concise one-for-one mapping of control symbols to high-level language constructs for purposes of design and documentation. The notation lends itself to both high-level and code-level algorithmic description. The various issues that may arise when representing, in D-Chart style, algorithms expressed in the more popular high-level languages are addressed. In particular, the peculiarities of mapping control constructs for Ada, PASCAL, FORTRAN 77, C, PL/I, Jovial J73, HAL/S, and Algol are discussed.

  4. GH Lib: A multi-periodic Mira, not an eclipsing binary

    Science.gov (United States)

    Siviero, Alessandro; Munari, Ulisse; Righetti, Gian Luigi; Graziani, Mauro

    2016-09-01

    Over the period 2012-2016 we have obtained accurate V and R band photometry and 3400-8000 Ang spectroscopy which show the poorly studied variable GH Lib to be a multi-periodic Mira and not an Algol-type eclipsing binary. The main pulsation periods are 157 and 1180 days, with amplitudes of 3.5 and 1.0 mag, respectively. The spectral type change from M2III at maximum to M7III at minimum. The intensity of Halpha and Hbeta emission lines in GH Lib is much larger than in normal Miras, suggesting that the region of Balmer line formation is located at a larger radius (more external atmospheric layers) as if mixed with and not deeply below the region where absorption by TiO molecules occurs.

  5. A numerical library in Java for scientists and engineers

    CERN Document Server

    Lau, Hang T

    2003-01-01

    At last researchers have an inexpensive library of Java-based numeric procedures for use in scientific computation. The first and only book of its kind, A Numeric Library in Java for Scientists and Engineers is a translation into Java of the library NUMAL (NUMerical procedures in ALgol 60). This groundbreaking text presents procedural descriptions for linear algebra, ordinary and partial differential equations, optimization, parameter estimation, mathematical physics, and other tools that are indispensable to any dynamic research group. The book offers test programs that allow researchers to execute the examples provided; users are free to construct their own tests and apply the numeric procedures to them in order to observe a successful computation or simulate failure. The entry for each procedure is logically presented, with name, usage parameters, and Java code included. This handbook serves as a powerful research tool, enabling the performance of critical computations in Java. It stands as a cost-effi...

  6. The Multiperiodic Pulsating Star Y Cam A as a Musical Instrument

    CERN Document Server

    Ulas, Burak

    2015-01-01

    In this study we generate musical chords from the oscillation frequencies of the primary component of oscillating eclipsing Algol system Y Cam. The parameters and the procedure of the musical chord generation process from the stellar oscillations are described in detail. A musical piece is also composed in appropriate scale for Y Cam A by using the generated chords from the results of the asteroseismic analysis of the stellar data. The music scores and the digital sound files are provided for both the generated chords and the musical composition. Our study shows that the further orchestral compositions can be made from the frequency analysis results of several pulsating stars by using the procedure stated in present study.

  7. Photometric Analysis and Period Investigation of the EW Type Eclipsing Binary V441 Lac

    Indian Academy of Sciences (India)

    K. Li; S.-M. Hu; D.-F. Guo; Y.-G. Jiang; D.-Y. Gao; X. Chen

    2016-09-01

    Four color light curves of the EW type eclipsing binary V441Lac were presented and analyzed by the W--D code. It is found that V441Lac is an extremely low mass ratio $(q = 0.093 \\pm 0.001)$ semi-detached binary with the less massive secondary component filling the inner Roche lobe. Two dark spots on the primary component were introduced to explain the asymmetric light curves. By analyzing all times of light minimum, we determined that the orbital period of V441 Lac is continuously increasing at a rate of ${\\rm d}P/{\\rm d}t = 5.874(\\pm 0.007)\\times 10^{--7} {\\rm d yr}^{--1}$. The semidetached Algol type configuration of V441 Lac is possibly formed by a contact configuration destroyed shallow contact binary due to mass transfer from the less massive component to the more massive one predicted by the thermal relaxation oscillation theory.

  8. Observations of an Eclipse of Bright Star b Persei by the Third Star in February 2013 (Abstract)

    Science.gov (United States)

    Collins, D. F.

    2013-12-01

    (Abstract only) b Persei (SAO 24531 = HD 26961, V ~4.52) is a multiple star system consisting of a close ellipsoidal binary with a 1.5-day period and a third star with a 702-day orbit. b Per is a non-thermal radio source, and the evolutionary stage of the close binary is unclear. It may be a non-eclipsing Algol or a precursor to the Algol stage. Observations with the Navy Precision Optical Interferometer showed that the third star has a nearly edge-on orbit about the close binary. Based on this orbit an eclipse of the close binary by the third star was predicted for late January 2013. A call for observations - especially those with equipment to observe bright stars instrumentally - was made via the AAVSO. With the "back yard" convenience of a DSLR camera on a fixed tripod, DFC obtained an observation of the V magnitude of b Persei nearly every clear night in January-February 2013. The DSLR clearly detected the expected eclipse with a drop in of 0.12 V on JD 2456329 and JD 2456330 (Feb 5-6, 2013 and Feb 6-7, 2013). The eclipse was also detected by other AAVSO observers extending to JD 2456331 inclusive. The estimated duration of the eclipse (FWHM) is 2.0 ± 0.3 d. The DSLR also detects the 1.53-day orbital period of the A and B components of b Persei - a variation of 0.05 V magnitude due to the non-eclipsing ellipsoidal star shapes. A concerted campaign should recruit many AAVSO observers to detect the next predicted eclipses in mid-January 2014 (secondary) and early January 2015 (primary) assuming a 702-day cycle. Future photometric observations may aid the understanding of the evolutionary stage of the close binary.

  9. Statistically Optimal Approximations of Astronomical Signals: Implications to Classification and Advanced Study of Variable Stars

    Science.gov (United States)

    Andronov, I. L.; Chinarova, L. L.; Kudashkina, L. S.; Marsakova, V. I.; Tkachenko, M. G.

    2016-06-01

    We have elaborated a set of new algorithms and programs for advanced time series analysis of (generally) multi-component multi-channel observations with irregularly spaced times of observations, which is a common case for large photometric surveys. Previous self-review on these methods for periodogram, scalegram, wavelet, autocorrelation analysis as well as on "running" or "sub-interval" local approximations were self-reviewed in (2003ASPC..292..391A). For an approximation of the phase light curves of nearly-periodic pulsating stars, we use a Trigonometric Polynomial (TP) fit of the statistically optimal degree and initial period improvement using differential corrections (1994OAP.....7...49A). For the determination of parameters of "characteristic points" (minima, maxima, crossings of some constant value etc.) we use a set of methods self-reviewed in 2005ASPC..335...37A, Results of the analysis of the catalogs compiled using these programs are presented in 2014AASP....4....3A. For more complicated signals, we use "phenomenological approximations" with "special shapes" based on functions defined on sub-intervals rather on the complete interval. E. g. for the Algol-type stars we developed the NAV ("New Algol Variable") algorithm (2012Ap.....55..536A, 2012arXiv1212.6707A, 2015JASS...32..127A), which was compared to common methods of Trigonometric Polynomial Fit (TP) or local Algebraic Polynomial (A) fit of a fixed or (alternately) statistically optimal degree. The method allows determine the minimal set of parameters required for the "General Catalogue of Variable Stars", as well as an extended set of phenomenological and astrophysical parameters which may be used for the classification. Totally more that 1900 variable stars were studied in our group using these methods in a frame of the "Inter-Longitude Astronomy" campaign (2010OAP....23....8A) and the "Ukrainian Virtual Observatory" project (2012KPCB...28...85V).

  10. Surprising Rapid Collapse of Sirius B from Red Giant to White Dwarf Through Mass Transfer to Sirius a

    Science.gov (United States)

    Yousef, Shahinaz; Ali, Ola

    2013-03-01

    Sirius was observed in antiquity as a red star. In his famous astronomy textbook the Almagest written 140 AD, Ptolemy described the star Sirius as fiery red. He curiously depicted it as one of six red-colored stars. The other five are class M and K stars, such as Arcturus and Betelgeuse. Apparent confirmation in ancient Greek and Roman sources are found and Sirius was also reported red in Europe about 1400 years ago. Sirius must have changed to a white dwarf in the night of Ascension. The star chapter in the Quran started with "by the star as it collapsed (1) your companion have not gone astray nor being misled (2), and in verse 49 which is the rotation period of the companion Sirius B around Sirius A, it is said" He is the Lord of Sirius (49). If Sirius actually was red what could have caused it to change into the brilliant bluish-white star we see today? What the naked eye perceives as a single star is actually a binary star system, consisting of a white main sequence star of spectral type A1V, termed Sirius A, and a faint white dwarf companion of spectral type DA2, termed Sirius B. The red color indicates that the star seen then was a red giant. It looks that what they have seen in antiquity was Sirius B which was then a red giant and it collapsed to form a white dwarf. Since there is no evidence of a planetary nebula, then the red Sirius paradox can be solved in terms of stellar evolution with mass transfer. Sirius B was the most massive star which evolved to a red giant and filled the Roche lobe. Mass transfer to Sirius A occurred through the Lagrangian point. Sirius A then became more massive while Sirius B lost mass and shrank. Sirius B then collapsed abruptly into a white dwarf. In the case of Algol, Ptolmy observed it as white star but it was red at the time of El sufi. At present it is white. The rate of mass transfer from Sirius B to Sirius A, and from Algol B to A is estimated from observational data of colour change from red to bullish white to be 0

  11. $\\gamma$ Doradus Pulsations in the Eclipsing Binary Star KIC 6048106

    CERN Document Server

    Lee, Jae Woo

    2016-01-01

    We present the ${\\it Kepler}$ photometry of KIC 6048106 exhibiting O'Connell effect and multiperiodic pulsations. Including a starspot on either of the components, light-curve synthesis indicates that this system is a semi-detached Algol with a mass ratio of 0.211, an orbital inclination of 73.9 deg, and a large temperature difference of 2,534 K. To examine in detail both spot variations and pulsations, we separately analyzed the {\\it Kepler} time-series data at the interval of an orbital period by an iterative way. The results reveal that the variable asymmetries of the light maxima can be interpreted as the changes of a magnetic cool spot on the secondary component with time. Multiple frequency analyses were performed in the outside-eclipse light residuals after removal of the binarity effects from the observed {\\it Kepler} data. We detected 30 frequencies with signal to noise amplitude ratios larger than 4.0, of which six ($f_2$--$f_6$ and $f_{10}$) can be identified as high-order (17 $\\le n \\le$ 25) low-d...

  12. KIC 8262223: A Post-Mass Transfer Eclipsing Binary Consisting of a Delta Scuti Pulsator and a Helium White Dwarf Precursor

    CERN Document Server

    Guo, Zhao; Matson, Rachel A; Hernández, Antonio García; Han, Zhanwen; Chen, Xuefei

    2016-01-01

    KIC~8262223 is an eclipsing binary with a short orbital period ($P=1.61$ d). The {\\it Kepler} light curves are of Algol-type and display deep and partial eclipses, ellipsoidal variations, and pulsations of Delta Scuti type. We analyzed the {\\it Kepler} photometric data, complemented by phase-resolved spectra from the R-C Spectrograph on the 4-meter Mayall telescope at Kitt Peak National Observatory and determined the fundamental parameters of this system. The low mass and oversized secondary ($M_2=0.20M_{\\odot}$, $R_2=1.31R_{\\odot}$) is the remnant of the donor star that transferred most of its mass to the gainer, and now the primary star. The current primary star is thus not a normal $\\delta$ Scuti star but the result of mass accretion from a lower mass progenitor. We discuss the possible evolutionary history and demonstrate with the MESA evolution code that the system can be understood as the result of non-conservative binary evolution similar to that for the formation of EL CVn type binaries. The pulsation...

  13. NSV 1907 - A new eclipsing, nova-like cataclysmic variable

    Science.gov (United States)

    Hümmerich, Stefan; Gröbel, Rainer; Hambsch, Franz-Josef; Dubois, Franky; Ashley, Richard; Gänsicke, Boris T.; Vanaverbeke, Siegfried; Bernhard, Klaus; Wils, Patrick

    2017-01-01

    NSV 1907, formerly listed as an irregular variable in variability catalogues, was classified as an Algol-type eclipsing binary in the Catalina Surveys Periodic Variable Star Catalogue. We have identified NSV 1907 as an ultraviolet (UV) bright source using measurements from the GALEX space telescope and detected obvious out-of-eclipse variability in archival photometric data from the Catalina Sky Survey, which instigated a closer examination of the object. A spectrum and extensive multicolour photometric observations were acquired, from which we deduce that NSV 1907 is a deeply eclipsing, nova-like cataclysmic variable. Apart from the orbital variations (deep eclipses with a period of P ≈ 6.63 hours), changes in mean brightness and irregular short-term variability (flickering) were observed. The presence of a secondary minimum at phase φ ≈ 0.5 was established, which indicates a significant contribution of the companion star to the optical flux of the system. We find possible evidence for sinusoidal variations with a period of P ≈ 4.2 d, which we interpret as the nodal precession period of the accretion disc. No outbursts or VY Scl-like drops in brightness were detected either by the CSS or during our photometric monitoring. Because of its spectral characteristics and the observed variability pattern, we propose NSV 1907 as a new moderately bright long-period SW Sextantis star. Further photometric and spectroscopic observations are encouraged.

  14. Phemenological Modeling of Eclipsing Binary Stars

    CERN Document Server

    Andronov, Ivan L; Chinarova, Lidia L

    2016-01-01

    We review the method NAV (New Algol Variable) first introduced in 2012Ap.....55..536A, which uses the locally-dependent shapes of eclipses in an addition to the trigonometric polynomial of the second order (which typically describes the "out-of-eclipse" part of the light curve with effects of reflection, ellipticity and O'Connell). Eclipsing binary stars are believed to show distinct eclipses only if belonging to the EA type. With a decreasing eclipse width, the statistically optimal value of the trigonometric polynomial s (2003ASPC..292..391A) drastically increases from ~2 for elliptic (EL) variables without eclipses, ~6-8 for EW and up to ~30-50 for some EA with narrow eclipses. In this case of large number of parameters, the smoothing curve becomes very noisy and apparent waves (the Gibbs phenomenon) may be seen. The NAV set of the parameters may be used for classification in the GCVS, VSX and similar catalogs. The maximal number of parameters is m=12, which corresponds to s=5, if correcting both the perio...

  15. Large X-ray Flares on Stars Detected with MAXI/GSC: A Universal Correlation between the Duration of a Flare and its X-ray Luminosity

    CERN Document Server

    Tsuboi, Yohko; Sugawara, Yasuharu; Kawagoe, Atsushi; Kaneto, Soichiro; Iizuka, Ryo; Matsumura, Takanori; Nakahira, Satoshi; Higa, Masaya; Matsuoka, Masaru; Sugizaki, Mutsumi; Ueda, Yoshihiro; Kawai, Nobuyuki; Morii, Mikio; Serino, Motoko; Mihara, Tatehiro; Tomida, Hiroshi; Ueno, Shiro; Negoro, Hitoshi; Daikyuji, Arata; Ebisawa, Ken; Eguchi, Satoshi; Hiroi, Kazuo; Ishikawa, Masaki; Isobe, Naoki; Kawasaki, Kazuyoshi; Kimura, Masashi; Kitayama, Hiroki; Kohama, Mitsuhiro; Kotani, Taro; Nakagawa, Yujin E; Nakajima, Motoki; Ozawa, Hiroshi; Shidatsu, Megumi; Sootome, Tetsuya; Sugimori, Kousuke; Suwa, Fumitoshi; Tsunemi, Hiroshi; Usui, Ryuichi; Yamamoto, Takayuki; Yamaoka, Kazutaka; Yoshida, Atsumasa

    2016-01-01

    23 giant flares from 13 active stars (eight RS CVn systems, one Algol system, three dMe stars and one YSO) were detected during the first two years of our all-sky X-ray monitoring with the gas propotional counters (GSC) of the Monitor of All-sky X-ray Image (MAXI). The observed parameters of all of these MAXI/GSC flares are found to be at the upper ends for stellar flares with the luminosity of 10^(31-34) ergs s-1 in the 2-20 keV band, the emission measure of 10^(54-57) cm-3, the e-folding time of 1 hour to 1.5 days, and the total radiative energy released during the flare of 10^(34-39) ergs. Notably, the peak X-ray luminosity of 5(3-9)*10^33 ergs s-1 in the 2-20 keV band was detected in one of the flares on II Peg, which is one of the, or potentially the, largest ever observed in stellar flares. X-ray flares were detected from GT Mus, V841 Cen, SZ Psc, and TWA-7 for the first time in this survey. Whereas most of our detected sources are multiple-star systems, two of them are single stars (YZ CMi and TWA-7). ...

  16. Time-series spectroscopy of the pulsating eclipsing binary XX Cephei

    CERN Document Server

    Koo, Jae-Rim; Hong, Kyeongsoo; Kim, Seung-Lee; Lee, Chung-Uk

    2016-01-01

    Oscillating Algol-type eclipsing binaries (oEA) are very interesting objects that have three observational features of eclipse, pulsation, and mass transfer. Direct measurement of their masses and radii from the double-lined radial velocity data and photometric light curves would be the most essential for understanding their evolutionary process and for performing the asteroseismological study. We present the physical properties of the oEA star XX Cep from high-resolution time-series spectroscopic data. The effective temperature of the primary star was determined to be 7,946 $\\pm$ 240 K by comparing the observed spectra and the Kurucz models. We detected the absorption lines of the secondary star, which had never been detected in previous studies, and obtained the radial velocities for both components. With the published $BVRI$ light curves, we determined the absolute parameters for the binary via Wilson-Devinney modeling. The masses and radii are $M_{1} = 2.49 \\pm 0.06$ $M_\\odot$, $M_{2} = 0.38 \\pm 0.01$ $M_...

  17. Modeling the Accretion Structure of AU Mon

    CERN Document Server

    Atwood-Stone, Corwin; Richards, Mercedes T; Budaj, Jan; Peters, Geraldine J

    2012-01-01

    AU Mon is a long-period (11.113 d) Algol-type binary system with a persistent accretion disk that is apparent as double-peaked H-alpha emission. We present previously unpublished optical spectra of AU Mon which were obtained over several years with dense orbital phase coverage. We utilize these data, along with archival UV spectra, to model the temperature and structure of the accretion disk and the gas stream. Synthetic spectral profiles for lines including H-alpha, H-beta, and the Al III and Si IV doublets were computed with the Shellspec program. The best match between the model spectra and the observations is obtained for an accretion disk of inner/outer radius 5.1/23 R_sun, thickness of 5.2 R_sun, density of 1.0e-13 g/cm^3, and maximum temperature of 14000 K, along with a gas stream at a temperature of ~8000 K transferring ~2.4e-9 M_sun/yr. We show H-alpha Doppler tomograms of the velocity structure of the gas, constructed from difference profiles calculated through sequentially subtracting contributions...

  18. The Kepler Eclipsing System KIC 5621294 and its Substellar Companion

    CERN Document Server

    Lee, Jae Woo; Hinse, Tobias Cornelius

    2014-01-01

    We present the physical properties of KIC 5621294 showing light and timing variations from the ${\\it Kepler}$ photometry. Its light curve displays partial eclipses and O'Connell effect with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. The results indicate that the eclipsing pair is a classical Algol-type system with parameters of $q$=0.22, $i$=76$^\\circ$.8, and $\\Delta$($T_{1}$--$T_{2}$)=4,235 K, in which the detached primary component fills about 77\\% of its limiting lobe. Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee \\& van Woerden. These are mainly caused by surface inhomogeneities due to spot activity detected in our light-curve synthesis. The 1,253 light-curve timings from the Wilson-Devinney code were used for a period study. It was found that the orbital period of KIC 5621294 has varied due to a periodic variation overlaid on a downward parabola. The sinusoidal variation ...

  19. A comprehensive photometric study of the eclipsing binary EP Aurigae

    Science.gov (United States)

    Li, H.-L.; Wei, J.-Y.; Yang, Y.-G.; Li, K.; Zhang, X.-B.

    2015-02-01

    We present new observations for the eclipsing binary EP Aurigae, which were performed by using three small telescopes in China from 2003 December to 2014 January. With the updated 2003 version of the Wilson-Devinney code, the photometric elements were deduced from three sets of light curves. Based on all available eclipsing times, the orbital period changes were investigated. It is discovered that the (O-C) curve may show an existence of light-time effect due to an unseen third body, which was weakly identified by the photometric solution. The modulated period and amplitude of the cyclic variation are P3=71.2(±8.0) yr and A=0.0101(±0.0008) day, respectively. In the co-planar orbit with the binary system, the mass of the third body is M3=0.18(±0.02) M⊙. The photometric results imply that EP Aur is an Algol-type binary with a mass ratio of q=0.831(±0.004). Its primary component almost fills its Roche lobe. Therefore, EP Aur may consist of a normal main-sequence star and a cool Roche-lobe filling subgiant, which may be undergoing rapid mass transfer.

  20. A Multiwavelength Study of RZ Cassiopeiae: The XMM-Newton/VLA Campaign

    CERN Document Server

    Audard, M; Güdel, M; Audard, Marc; Donisan, Julius R.; Guedel, Manuel

    2004-01-01

    XMM-Newton and the VLA simultaneously observed the eclipsing Algol-type binary RZ Cassiopeiae in August 2003. The secondary eclipse (K3 IV companion behind the A3 V primary) was placed at the center of the 15-hour radio campaign, while the X-ray satellite monitored a full 1.2-day orbital period. We present results of the X-ray and radio campaigns. The X-ray light curve shows significant modulation probably related to rotational modulation and active region evolution, and even small flares. However, the X-ray eclipse is not deep, implying that the coronal X-ray emitting material is spatially extended. The Reflection Grating Spectrometer (RGS) spectrum shows a variety of bright emission lines from Fe, Ne, O, N. A strong [C/N] depletion probably reflects the surface composition of the secondary which fills its Roche lobe and loses material onto the primary. The O~\\textsc{vii} He-like triplet reflects a low forbidden-to-intercombination ratio; while it generally suggests high electron densities, the ratio is here...

  1. Das Universum der Sterne. Himmelsbeobachtungen und Streifzüge durch die moderne Astronomie.

    Science.gov (United States)

    Rowan-Robinson, M.

    This book is a German translation, by M. Röser, of the English original published in 1990 (see 52.003.046). Contents: 1. Der Halleysche Komet. 2. Alpha Centauri - Der sonnennächste Stern. 3. Sirius und sein Begleiter, ein Weißer Zwerg. 4. Polaris - Der Polarstern. 5. Wega - Ein Planetensystem im Entstehen? 6. Mira - Der erste bekannte veränderliche Stern. 7. Der Ring-Nebel - "Todeskampf" eines sonnenähnlichen Sterns. 8. Der Orion-Nebel - Die Geburt neuer Sterne. 9. Delta Cephei - Die Meßlatte des Weltalls. 10. Algol - Der Teufelsstern. 11. Nova Aquilae - Der neue Stern von 1918. 12. Der Krebs-Nebel - Die Supernova des Jahres 1054. 13. Die Hyaden und Plejaden - Sternhaufen. 14. Die Milchstraße - Unsere Galaxis. 15. Die Magellanschen Wolken - Unsere Nachbarn im Weltall. 16. Der Andromeda-Nebel - Zwilling unserer Galaxis. 17. Messier 87 - Eine Radiogalaxie. 18. 3C 273 - Rätselhafter Quasar. 19. Messier 82 - Eine "Starburst"-Galaxie. 20. Der Virgo-Haufen - Ein reicher Galaxienhaufen. 21. Das Universum.

  2. IUE spectroscopy of U Cephei during the mass flow outburst of 1986 June

    Science.gov (United States)

    Mccluskey, George E., Jr.; Kondo, Yoji; Olson, Edward C.

    1988-01-01

    The interacting Algol-type binary U Cep underwent another of its irregularly occurring transient high-mass flow events during June 1986. For the first time, high-resolution ultraviolet spectroscopy of U Cep during such an event was possible. High-resolution spectra in the far-ultraviolet and near-ultraviolet were obtained with IUE. These spectra show that the ultraviolet continuum decreased by factors of 1.2 to 3.0 during the greatest activity. In addition, one or more narrow absorption components with radial velocities as high as -500 km/s appeared in association with a number of C, Si, Al, Fe, Zn, and Mg lines. The Mg II doublet developed a flat-bottomed appearance with a residual intensity of about 0.31 and a width of at least 800 km/s. These phenomena are interpreted in terms of high-velocity gas streams, mass loss from the system, and the formation of an optically thick equatorial bulge around the B star.

  3. Light Curve and Orbital Period Analysis of VX Lac

    Science.gov (United States)

    Yılmaz, M.; Nelson, R. H.; Şenavcı, H. V.; İzci, D.; Özavcı, İ.; Gümüş, D.

    2017-04-01

    In this study, we performed simultaneously light curve and radial velocity, and also period analyses of the eclipsing binary system VX Lac. Four color (BVRI) light curves of the system were analysed using the W-D code. The results imply that VX Lac is a classic Algol-type binary with a mass ratio of q=0.27, of which the less massive secondary component fills its Roche lobe. The orbital period behaviour of the system was analysed by assuming the light time effect (LITE) from a third body. The O-C analysis yielded a mass transfer rate of dM/dt=1.86×10-8Mȯyr-1 and the minimal mass of the third body to be M3=0.31Mȯ. The residuals from mass transfer and the third body were also analysed because another cyclic variation is seen in O-C diagram. This periodic variation was examined under the hypotheses of stellar magnetic activity and fourth body.

  4. Complex Analysis of the Stellar Binary V446\\,Cep; A New Massive Eclipsing Binary in Cepheus\\,OB2 Association

    CERN Document Server

    Cakirli, O; Sipahi, E; Frasca, A; Catanzaro, G

    2014-01-01

    We present new spectroscopic observations of the early type, double-lined eclipsing binary V446\\,Cep. The radial velocities and the photometric data obtained by $Hipparcos$ were analysed for deriving the astrophysical parameters of the components. Masses and radii were determined as M$_p$=17.94$\\pm$1.16 M$_{\\odot}$ and R$_p$=8.33$\\pm$0.29 R$_{\\odot}$, M$_s$=2.64$\\pm$0.30 M$_{\\odot}$ and R$_s$=2.13$\\pm$0.10 R$_{\\odot}$ for the components of V446\\,Cep. Our analyses show that V446\\,Cep is a detached Algol-type system. Based on the position of the components plotted on the theoretical Hertzsprung-Russell diagram, we estimate that the age of V446\\,Cep is about 10 Myr, neglecting the effects of mass-loss and mass exchange between the components. Using the UBVJHK magnitudes and interstellar absorption we estimated the mean distance to the system V446\\,Cep as 1100$\\pm$62\\,pc.

  5. Period change and δ Scuti pulsations of eclipsing binary star RZ Cassiopiae

    Directory of Open Access Journals (Sweden)

    K Naficy

    2009-12-01

    Full Text Available RZ Cas is an Algol-type partial eclipsing binary, the secondary component of which has filled its Roche lobe. Its visual magnitude is 6.18 and its period is 1.195 days. The most important characteristics of RZ Cas are period change (due to mass transfer and anomalies in the primary minimum of its light curve (due to δ Scuti pulsations. In this paper, light curves of RZ Cas are obtained using the Johnson's U, B, V, and R filters at Isfahan University Observatory, and B and V filters at Biruni Observatory of Shiraz University. Continuous photometric measurements have also been made to detect δ Scuti type pulsations. A new ephemeris and period is obtained: Min.I =HJD2453620.5500 + 1d.1952639 E, and a mass transfer rate of 1.5×10 -7 M⊙ yr -1 is estimated. None of the observed primary minima is flat as found by some observers before. The residuals from the observed minus computed light curves of the system give the pulsation light curves of the primary component. The frequencies of δ Scuti pulsation are searched for using the Period04 program. It is found that the dominant frequency is 65.5-68.5 cycle/day, corresponding to a period of 21-22 min.

  6. A Spectroscopic Study of Kepler Asteroseismic Targets

    CERN Document Server

    Molenda-Zakowicz, J; Latham, D W; Jerzykiewicz, M

    2009-01-01

    Reported are spectroscopic observations of 15 candidates for Kepler primary asteroseismic targets and 14 other stars in the Kepler field, carried out at three observatories (see the footnote). For all these stars, the radial velocities, effective temperature, surface gravity, metallicity, and the projected rotational velocity are derived from two separate sets of data by means of two independent methods. In addition, MK type is estimated from one of these sets of data. Three stars, HIP 94335, HIP 94734, and HIP 94743, are found to have variable radial-velocity. For HIP 94335 = FL Lyr, a well-known Algol-type eclipsing variable and a double-lined spectroscopic binary, the orbital elements computed from our data agree closely with those of Popper et al. For HIP 94734 and HIP 94743 = V2077 Cyg, which we discover to be single-lined systems, orbital elements are derived. In addition, from our value of the orbital period and the Hipparcos epoch photometry, HIP 94743 is demonstrated to be a detached eclipsing binary...

  7. Milliarcsecond radio structure of weak-lined T Tauri stars

    Science.gov (United States)

    Phillips, R. B.; Lonsdale, C. J.; Feigelson, E. D.

    1991-01-01

    VLBI and VLA observations of six radio-bright weak-lined T Taur (WTT) stars are reported, as well as direct measurements of the sizes of the emitting regions. VLBI measurements established that essentially all the radio emission from these premain-sequence stars originates in regions 15 stellar radii or less in size. Corresponding brightness temperatures ranged from 10 exp 7.5 to not less than 10 exp 9 K, ruling out a thermal process such as free-free bremsstrahlung radiation from a circumstellar wind. The radio luminosity and structure of several stars changed significantly between measurements separated by 1 day. HD 283447 showed intraday radio variability on time scales as short as 1 hr. Corresponding VLBI measurements show a new unresolved component appearing after an increase in flux density, possibly indicating that the driving agent for larger radio flares originates close to the star. The high conformation rate of nonthermal radio emission from this initial sample of radio-bright WTT stars show that these solar-type premain-sequence stars alter their immediate environments via magnetic processes to an extent comparable to that shown by RS CVn or Algol close binaries.

  8. Automated classification of periodic variable stars detected by the wide-field infrared survey explorer

    Energy Technology Data Exchange (ETDEWEB)

    Masci, Frank J.; Grillmair, Carl J.; Cutri, Roc M. [Infrared Processing and Analysis Center, Caltech 100-22, Pasadena, CA 91125 (United States); Hoffman, Douglas I., E-mail: fmasci@ipac.caltech.edu [NASA Ames Research Center, Moffett Field, CA 94035 (United States)

    2014-07-01

    We describe a methodology to classify periodic variable stars identified using photometric time-series measurements constructed from the Wide-field Infrared Survey Explorer (WISE) full-mission single-exposure Source Databases. This will assist in the future construction of a WISE Variable Source Database that assigns variables to specific science classes as constrained by the WISE observing cadence with statistically meaningful classification probabilities. We have analyzed the WISE light curves of 8273 variable stars identified in previous optical variability surveys (MACHO, GCVS, and ASAS) and show that Fourier decomposition techniques can be extended into the mid-IR to assist with their classification. Combined with other periodic light-curve features, this sample is then used to train a machine-learned classifier based on the random forest (RF) method. Consistent with previous classification studies of variable stars in general, the RF machine-learned classifier is superior to other methods in terms of accuracy, robustness against outliers, and relative immunity to features that carry little or redundant class information. For the three most common classes identified by WISE: Algols, RR Lyrae, and W Ursae Majoris type variables, we obtain classification efficiencies of 80.7%, 82.7%, and 84.5% respectively using cross-validation analyses, with 95% confidence intervals of approximately ±2%. These accuracies are achieved at purity (or reliability) levels of 88.5%, 96.2%, and 87.8% respectively, similar to that achieved in previous automated classification studies of periodic variable stars.

  9. Images of Gravitational and Magnetic Phenomena Derived from 2D Back-Projection Doppler Tomography of Interacting Binary Stars

    CERN Document Server

    Richards, Mercedes T; Fisher, John G; Conover, Marshall J

    2014-01-01

    We have used 2D back-projection Doppler tomography as a tool to examine the influence of gravitational and magnetic phenomena in interacting binaries which undergo mass transfer from a magnetically-active star onto a non-magnetic main sequence star. This multi-tiered study of over 1300 time-resolved spectra of 13 Algol binaries involved calculations of the predicted dynamical behavior of the gravitational flow and the dynamics at the impact site, analysis of the velocity images constructed from tomography, and the influence on the tomograms of orbital inclination, systemic velocity, orbital coverage, and shadowing. The H$\\alpha$ tomograms revealed eight sources: chromospheric emission, a gas stream along the gravitational trajectory, a star-stream impact region, a bulge of absorption or emission around the mass-gaining star, a Keplerian accretion disk, an absorption zone associated with hotter gas, a disk-stream impact region, and a hot spot where the stream strikes the edge of a disk. We described several me...

  10. An Orbital Stability Study of the Proposed Companions of SW Lyncis

    CERN Document Server

    Hinse, Tobias C; Wittenmyer, Robert A

    2014-01-01

    We have investigated the dynamical stability of the proposed companions orbiting the Algol type short-period eclipsing binary SW Lyncis (Kim et al. 2010). The two candidate companions are of stellar to sub-stellar nature, and were inferred from timing measurements of the system's primary and secondary eclipses. We applied well-tested numerical techniques to accurately integrate the orbits of the two companions and to test for chaotic dynamical behaviour. We carried out the stability analysis within a systematic parameter survey varying both the geometries and orientation of the orbits of the companions, as well as their masses. In all our numerical integrations we found that the proposed SW Lyn multi-body system is highly unstable on time-scales on the order of 1000 years. Our results cast doubt on the interpretation that the timing variations are caused by two companions. This work demonstrates that a straightforward dynamical analysis can help to test whether a best-fit companion-based model is a physically...

  11. An incisive look at the symbiotic star SS Leporis -- Milli-arcsecond imaging with PIONIER/VLTI

    CERN Document Server

    Blind, N; Berger, J -P; Bouquin, J -B Le; Mérand, A; Lazareff, B; Zins, G; 10.1051/0004-6361/201118036

    2011-01-01

    Context. Determining the mass transfer in a close binary system is of prime importance for understanding its evolution. SS Leporis, a symbiotic star showing the Algol paradox and presenting clear evidence of ongoing mass transfer, in which the donor has been thought to fill its Roche lobe, is a target particularly suited to this kind of study. Aims. Since previous spectroscopic and interferometric observations have not been able to fully constrain the system morphology and characteristics, we go one step further to determine its orbital parameters, for which we need new interferometric observations directly probing the inner parts of the system with a much higher number of spatial frequencies. Methods. We use data obtained at eight different epochs with the VLTI instruments AMBER and PIONIER in the H- and K-bands. We performed aperture synthesis imaging to obtain the first model-independent view of this system. We then modelled it as a binary (whose giant is spatially resolved) that is surrounded by a circumb...

  12. V1898 CYGNI: AN INTERACTING ECLIPSING BINARY IN THE VICINITY OF NORTH AMERICA NEBULA

    Directory of Open Access Journals (Sweden)

    A. Dervisoglu

    2011-01-01

    Full Text Available Presentamos observaciones espectroscópicas de la binaria eclipsante tipo Algol, de doble línea, V1898 Cygni. El análisis de las curvas de luz en las bandas BV nos lleva a una determinación de los parmetros fundamentales de las componentes de V1898 Cygni. Los parámetros absolutos son: M1 = 6.054 ± 0.037 M, M2 = 1.162 ± 0.011 M, R1 = 3.526 ± 0.009 R, R2 = 2.640 ± 0.010 R, Teff1 = 18000 ± 600 K, y Teff2 = 6200 ± 200 K. Analizamos los residuos entre los tiempos observados y calculados para el eclipse medio y obtenemos una tasa de cambio del periodo de P /P = 6.68×107 yr1. Estimamos una tasa de transferencia de masa de 1.88×107 M¿ por año. Utilizando las magnitudes infrarojas JHK y las correcciones bolométricas para la estrella primaria, calculamos la distancia al sistema V1898 Cyg como 501 ±5 pc. Las componentes de los movimientos propios del sistema presentan alguna información sobre su pertenencia a la Nebulosa de Norteamérica.

  13. UX Ori Variables in the Cluster IC 348

    Science.gov (United States)

    Barsunova, O. Yu.; Grinin, V. P.; Sergeev, S. G.; Semenov, A. O.; Shugarov, S. Yu.

    2015-06-01

    Results are presented from many years of photometric (VRCIC) observations of three variable T Tauri type stars in the cluster IC 348: V712 Per, V719 Per, and V909 Per. All three stars have photometric activity characteristic of UX Ori stars. The activity of V719 Per has increased significantly over the last 10 years: the amplitude of its Algol-like minima has increased by roughly a factor of 4 and has reached three stellar magnitudes in the I band. Periodograms of the light curves do not confirm the periods found previously by other authors on the basis of shorter series of observations. The slope of the color tracks on "color-magnitude" diagrams is used to determine the reddening law for these stars owing to selective absorption by circumstellar dust. Modelling of these parameters by the Mie theory shows that the maximum size amax of the dust particles in the protoplanetary disks of these stars is 1.5-2 times greater than in the interstellar medium. In V712 Per and V909 Per, the bulk of the mass of the dust particles is concentrated near amax, while in V719 Per the average mass of the dust particles is determined by the minimum size of the particles. It should be emphasized that these conclusions rely on an analysis of the optical variability of these stars.

  14. Evidence for quasiperiodicity in orbital period modulation of WW Cygni

    Science.gov (United States)

    Pop, Alexandru; Crăciun, Maria; Mocanu, Gabriela Raluca; Vamoş, Călin

    2017-04-01

    The Algol type binary system WW Cygni is known to display an intricate orbital period variability phenomenon which consists in the presence of an alternating component superposed on a secular trend. The alternating component clearly deviates from a strictly periodic pattern. In the present paper we studied WW Cyg using a data set consisting of 309 times of primary minimum, free of outliers, covering a time base of 113.8 yr. We investigated these timing data using periodicity detection methods relying on both amplitude spectrum and enhanced self-correlation (ESC) methods through Monte Carlo simulations. The problem of estimation of the statistical significance in the ESC method was further developed. The multiperiodicity of the O-C residuals was investigated via iterative prewhitening using three types of models consisting of polynomial (P) + multiperiodic (MP) terms, P + light travel time effect (LTTE) terms, and P + MP terms + LTTE terms. The interpretation of the results led us to the following two hypotheses: (i) a quasiperiodic modulation at a time scale of about 46 yr induced by the cyclic magnetic activity occurring in the cool secondary component of WW Cyg, or (ii) the coexistence of a periodic modulation with a period of 50.41 yr related to the presence of an unseen compact stellar object of at least 2.22 M_{⊙} in the system and a quasiperiodic modulation at a time scale of about 19.7 yr, caused by the mechanism (i).

  15. Evolution in Binary and Triple Stars, with an application to SS Lac

    CERN Document Server

    Eggleton, P P; Eggleton, Peter P.; Kiseleva-Eggleton, Ludmila

    2001-01-01

    We present equations governing the way in which both the orbit and the intrinsic spins of stars in a close binary should evolve subject to a number of perturbing forces, including the effect of a third body in a possibly inclined wider orbit. We illustrate the solutions in some binary-star and triple-star situations: tidal friction in a wide but eccentric orbit of a radio pulsar about a B star, the Darwin and eccentricity instabilities in a more massive but shorter-period massive X-ray binary, and the interaction of tidal friction with Kozai cycles in a triple such as Algol (beta-Per), at an early stage in that star's life when all 3 components were ZAMS stars. We also attempt to model in some detail the interesting triple system SS Lac, which stopped eclipsing in about 1950. We find that our model of SS Lac is quite constrained by the relatively good observational data of this system, and leads to a specific inclination (29 deg) of the outer orbit relative to the inner orbit at epoch zero (1912). Although th...

  16. First results from the RAO Variable Star Search Program: I. Background, Procedure, and Results from RAO Field 1

    CERN Document Server

    Williams, Michael D

    2011-01-01

    We describe an ongoing variable star search program and present the first reduced results of a search in a 19 square degree (4.4\\circle x 4.4\\circle) field centered on J2000 {\\alpha} = 22:03:24, {\\delta} = +18:54:32. The search was carried out with the Baker-Nunn Patrol Camera located at the Rothney Astrophysical Observatory in the foothills of the Canadian Rockies. A total of 26,271 stars were detected in the field, over a range of about 11-15 (instrumental) magnitudes. Our image processing made use of the IRAF version of the DAOPHOT aperture photometry routine and we used the ANOVA method to search for periodic variations in the light curves. We formally detected periodic variability in 35 stars, that we tentatively classify according to light curve characteristics: 6 EA (Algol), 5 EB ({\\beta} Lyrae), 19 EW (W UMa), and 5 RR (RR Lyrae) stars. Eleven of the detected variable stars have been reported previously in the literature. The eclipsing binary light curves have been analyzed with a package of light cur...

  17. Mathematical model of various statements of C-type Language

    Directory of Open Access Journals (Sweden)

    Manoj Kumar Srivastav

    2013-12-01

    Full Text Available Some of the important components of high level languages are statements, keywords, variable declarations, arrays, user defined functions etc. In case of object oriented programming language we use class, object, inheritance, operator overloading, function overloading, polymorphism etc. There are some common category of statements such as control statement, loop statements etc. Pointers are also one important concept in C-language. User defined functions, function subprograms or subroutines are also important concepts in different programming languages. The language like ALGOL was developed using Chomsky context free grammar. The similar concept used in C-type languages. The high level languages are now based on mathematical derivations and logic. Most of the components of any high level language can be obtained from simple mathematical logic and derivations. In the present study the authors have tried to give some unified mathematical model of few statements, arrays, user defined functions of C-language. However, the present method may further be extended to any other high level language.

  18. TIME-SERIES SPECTROSCOPY OF THE ECLIPSING BINARY Y CAM WITH A PULSATING COMPONENT

    Energy Technology Data Exchange (ETDEWEB)

    Hong, Kyeongsoo; Lee, Jae Woo; Kim, Seung-Lee; Koo, Jae-Rim; Lee, Chung-Uk [Korea Astronomy and Space Science Institute, Daejeon 305-348 (Korea, Republic of); Yushchenko, Alexander V.; Kang, Young-Woon, E-mail: kshong@kasi.re.kr [Department of Astronomy and Space Science, Sejong University, Seoul, 143-747 (Korea, Republic of)

    2015-10-15

    We present the physical properties of the semi-detached Algol-type eclipsing binary Y Cam based on high resolution spectra obtained using the Bohyunsan Optical Echelle Spectrograph. This is the first spectroscopic monitoring data obtained for this interesting binary system, which has a δ Sct-type pulsating component. We obtained a total of 59 spectra over 14 nights from 2009 December to 2011 March. Double-lined spectral features from the hot primary and cool secondary components were well identified. We determined the effective temperatures of the two stars to be T{sub eff,1} = 8000 ± 250 K and T{sub eff,2} = 4629 ± 150 K. The projected rotational velocities are v{sub 1}sin i{sub 1} = 51 ± 4 km s{sup −1} and v{sub 2}sin i{sub 2} = 50 ± 10 km s{sup −1}, which are very similar to a synchronous rotation with the orbital motion. Physical parameters of each component were derived by analyzing our radial velocity data together with previous photometric light curves from the literature. The masses and radii are M{sub 1} = 2.08 ± 0.09 M{sub ⊙}, M{sub 2} = 0.48 ± 0.03 M{sub ⊙}, R{sub 1} = 3.14 ± 0.05 R{sub ⊙}, and R{sub 2} = 3.33 ± 0.05 R{sub ⊙}, respectively. A comparison of these parameters with the theoretical evolution tracks showed that the primary component is located between the zero-age main sequence and the terminal-age main sequence, while the low-mass secondary is noticeably evolved. This indicates that the two components have experienced mass exchange with each other and the primary has undergone an evolution process different from that of single δ Sct-type pulsators.

  19. The Kepler eclipsing system KIC 5621294 and its substellar companion

    Energy Technology Data Exchange (ETDEWEB)

    Lee, Jae Woo; Hong, Kyeongsoo; Hinse, Tobias Cornelius, E-mail: jwlee@kasi.re.kr, E-mail: kshong@kasi.re.kr, E-mail: tchinse@gmail.com [Korea Astronomy and Space Science Institute, Daejeon 305-348 (Korea, Republic of)

    2015-03-01

    We present the physical properties of KIC 5621294, showing light and timing variations from the Kepler photometry. Its light curve displays partial eclipses and the O’Connell effect, with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. The results indicate that the eclipsing pair is a classical Algol-type system with parameters of q = 0.22, i = 76.°8, and Δ(T{sub 1}−T{sub 2}) = 4235 K, in which the detached primary component fills about 77% of its limiting lobe. Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee and van Woerden. These are mainly caused by surface inhomogeneities due to spot activity detected in our light curve synthesis. The 1253 light curve timings from the Wilson–Devinney code were used for a period study. It was found that the orbital period of KIC 5621294 has varied due to periodic variation overlaid on a downward parabola. The sinusoidal variation with a period of 961 days and a semi-amplitude of 22.5 s most likely arises from a light-time effect due to a third component with a mass of M{sub 3}sini{sub 3} = 46.9 M{sub Jup}, which is in good agreement with that calculated from the light curve itself. If its orbital inclination is larger than about 40°, the mass of the circumbinary object would possibly match a brown dwarf. The parabolic variation could not be fully explained by either a mass transfer between the binary components or angular momentum via magnetic braking. It is possible that the parabola may be the only observed part of a period modulation caused by the presence of another companion in a wider orbit.

  20. Invited Talk: Photometry of Bright Variable Stars with the BRITE Constellation Nano-Satellites: Opportunities for Amateur Astronomers

    Science.gov (United States)

    Guinan, E. F.

    2014-06-01

    (Abstract only) The BRIght Target Explorer (BRITE) is a joint Austrian-Canadian-Polish Astronomy mission to carry out high precision photometry of bright (mv computers, and so on. The first two (of up to six) satellites were successfully launched during February 2013. After post-launch commissioning, science operations commenced during October 2013. The primary goals are to carry out continuous multi-color (currently blue and red filters) high-precision millimag (mmag) photometry in particular locations in the sky. Typically these pointings will last for two to four months and secure simultaneous blue/red photometry of bright variable stars within the field. The first science pointing is centered on the Orion region. Since most bright stars are intrinsically luminous, hot O/B stars, giants, and supergiants will be the most common targets. However, some bright eclipsing binaries (such as Algol, b Lyr, e Aur) and a few chromospherically-active RS CVn stars (such as Capella) may be eventually be monitored. The BRITE-Constellation program of high precision, two color photometry of bright stars offers a great opportunity to study a wide range of stellar astrophysical problems. Bright stars offer convenient laboratories to study many current and important problems in stellar astrophysics. These include probing stellar interiors and pulsation in pulsating stars, tests of stellar evolution and structure for Cepheids and other luminous stars. To scientifically enhance the BRITE science returns, the BRITE investigators are very interested in securing contemporaneous ground-based spectroscopy and standardized photometry of target stars. The BRITE Ground Based Observations Team is coordinating ground-based observing efforts for BRITE targets. The team helps coordinate collaborations with amateur and professional astronomer. The ground-based coordinators are: Thomas Eversberg (thomas.eversberg@dlr.de) and, for spectroscopy, Contanze Zwintz (konstanze@ster.kuleuven.be). Detailed

  1. The Near-contact Binary RZ Draconis with Two Possible Light-time Orbits

    Science.gov (United States)

    Yang, Y.-G.; Li, H.-L.; Dai, H.-F.; Zhang, L.-Y.

    2010-12-01

    We present new multicolor photometry for RZ Draconis, observed in 2009 at the Xinglong Station of the National Astronomical Observatories of China. By using the updated version of the Wilson-Devinney Code, the photometric-spectroscopic elements were deduced from new photometric observations and published radial velocity data. The mass ratio and orbital inclination are q = 0.375(±0.002) and i = 84fdg60(±0fdg13), respectively. The fill-out factor of the primary is f = 98.3%, implying that RZ Dra is an Algol-like near-contact binary. Based on 683 light minimum times from 1907 to 2009, the orbital period change was investigated in detail. From the O - C curve, it is discovered that two quasi-sinusoidal variations may exist (i.e., P 3 = 75.62(±2.20) yr and P 4 = 27.59(±0.10) yr), which likely result from light-time effects via the presence of two additional bodies. In a coplanar orbit with the binary system, the third and fourth bodies may be low-mass drafts (i.e., M 3 = 0.175 M sun and M 4 = 0.074 M sun). If this is true, RZ Dra may be a quadruple star. The additional body could extract angular momentum from the binary system, which may cause the orbit to shrink. With the orbit shrinking, the primary may fill its Roche lobe and RZ Dra evolves into a contact configuration.

  2. The Kepler Eclipsing System KIC 5621294 and Its Substellar Companion

    Science.gov (United States)

    Lee, Jae Woo; Hong, Kyeongsoo; Hinse, Tobias Cornelius

    2015-03-01

    We present the physical properties of KIC 5621294, showing light and timing variations from the Kepler photometry. Its light curve displays partial eclipses and the O’Connell effect, with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. The results indicate that the eclipsing pair is a classical Algol-type system with parameters of q = 0.22, i = 76.°8, and Δ(T1-T2) = 4235 K, in which the detached primary component fills about 77% of its limiting lobe. Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee & van Woerden. These are mainly caused by surface inhomogeneities due to spot activity detected in our light curve synthesis. The 1253 light curve timings from the Wilson-Devinney code were used for a period study. It was found that the orbital period of KIC 5621294 has varied due to periodic variation overlaid on a downward parabola. The sinusoidal variation with a period of 961 days and a semi-amplitude of 22.5 s most likely arises from a light-time effect due to a third component with a mass of {{M}3}sin {{i}3} = 46.9 MJup, which is in good agreement with that calculated from the light curve itself. If its orbital inclination is larger than about 40°, the mass of the circumbinary object would possibly match a brown dwarf. The parabolic variation could not be fully explained by either a mass transfer between the binary components or angular momentum via magnetic braking. It is possible that the parabola may be the only observed part of a period modulation caused by the presence of another companion in a wider orbit.

  3. Two particular EA-type binaries in the globular cluster ω Centauri

    Institute of Scientific and Technical Information of China (English)

    Kai Li; Sheng-Bang Qian

    2013-01-01

    We analyzed the B and V light curves of two EA-type binaries V211 and NV358 for the first time using the Wilson-Devinney code.Our analysis shows that V211 is a typical Algol-type binary and NV358 is a well detached binary system.As the two binaries are definite members of ω Centauri due to their proper motion,we estimated their physical parameters,obtaining M1 =1.13 ± 0.03 M⊙,R1 =0.98 ± 0.01 R⊙,M2 =0.33 ± 0.01 M⊙ and R2 =0.92 ± 0.01 R⊙ for V211;M1 =1.30±0.05 M⊙,R1 =1.03±0.01 R⊙,M2 =0.58±0.02 M⊙ and R2 =0.78±0.01 R⊙ for NV358.On the color-magnitude diagram of ω Centauri,V211 is located in the faint blue straggler region and its primary component is more massive than a star at the main-sequence turnoff.Therefore,V211 is a blue straggler and was formed by mass transfer from the secondary component to the primary.The age of NV358is less than 1.93 Gyr,indicating that it is much younger than the first generation of stars in ω Centauri.Like NV364 in ω Centauri,NV358 should be a second-generation binary.

  4. Photometric and Polarimetric Activity of the Herbig Ae Star VX Cas

    Science.gov (United States)

    Shakhovskoi, D. N.; Rostopchina, A. N.; Grinin, V. P.; Minikulov, N. Kh.

    2003-04-01

    We present the results of our simultaneous photometric and polarimetric observations of the Herbig Ae/Be star VX Cas acquired in 1987 2001. The star belongs to the UX Ori subtype of young variable stars and exhibits a rather low level of photometric activity: only six Algol-like minima with amplitudes ΔV>1m were recorded in 15 years of observations. Two of these minima, in 1998 and 2001, were the deepest in the history of the star’s photometric studies, with V amplitudes of about 2m. In each case, the dimming was accompanied by an increase in the linear polarization in agreement with the law expected for variable circumstellar extinction. The highest V polarization was about 5%. Observations of VX Cas in the deep minima revealed a turnover of the color tracks, typical of stars of this type and due to an increased contribution from radiation scattered in the circumstellar disk. We separated the observed polarization of VX Cas into interstellar (P is) and intrinsic (P in) components. Their position angles differ by approximately 60°, with P is dominating in the bright state and P in dominating during the deep minima. The competition of these two polarization components leads to changes in both the degree and position angle of the polarization during the star’s brightness variations. Generally speaking, in terms of the behavior of the brightness, color indices, and linear polarization, VX Cas is similar to other UX Ori stars studied by us earlier. A number of episodes of photometric and polarimetric activity suggest that, in their motion along highly eccentric orbits, circumstellar gas and dust clouds can enter the close vicinity of the star (and be disrupted there).

  5. Light curve analysis of GSC 2750-0054 and GSC 03208-02644

    Science.gov (United States)

    Elkhateeb, M. M.; Nouh, M. I.

    2016-11-01

    We present the first photometric analysis for the newly discovered eclipsing binary systems of Algole-type GSC 2750-0054 and GSC 03208-02644. Our analysis was carried out by means of the most recent version of Wilson Devinney (WD) code, which applies the model atmosphere by (Kurucz, R., 1993. In: Milon, E. (Ed.), Light Curve Modeling of Eclipsing Binary Stars. Springer-Verlag, New York, p. 93) with a prescription in passband for the radiative treatment. The accepted light curve solutions reveal absolute physical parameters and the spectral classifications for the components are adopted. We derived the spectral types of the system GSC 2750-0054 as K3 and K7. The physical parameters of the system are M1 = 0.72 ± 0.03 M⊙, M2 = 0.47 ± 0.02 M⊙, R1 = 0.81 ± 0.03 R⊙, R2 = 0.62 ± 0.03 R⊙, L1 = 0.27 ± 0.01 L⊙ and L2 = 0.1 ± 0.004 L⊙. For the system, GSC 03208 02644 the spectral types of the components are A5 and A8. The physical parameters are M1 = 1.86 ± 0.076 M⊙, M2 = 1.21 ± 0.049 M⊙, R1 = 1.84 ± 0.075 R⊙, R2 = 1.75 ± 0.072 R⊙, L1 = 13.58 ± 0.55 L⊙ and L2 = 9.94 ± 0.41 L⊙. Comparison with the evolutionary models as well as the empirical databases is presented.

  6. Photometric activity of the Herbig Be star MWC 297 over 25 years

    Science.gov (United States)

    Barsunova, O. Yu.; Mel'nikov, S. Yu.; Grinin, V. P.; Katysheva, N. A.; Shugarov, S. Yu.

    2013-02-01

    The photometric behavior of the hot, young Herbig Be starMWC 297 on various time scales is studied using published data, as well as new observations. The series of photometric observations covers about 25 years. Over this time, the star showed low-amplitude (Δ V ≈ 0.3 m ) irregular variabilitymodulated by large-scale cyclic variabilitywith an amplitude close to 0.2 m and a period (or quasi-period) of 5.4±0.1 yr. A detailed seasonal analysis of the data shows that the light curve of MWC 297 displays two types of photometric features: low-amplitude Algol-like fading with an amplitude close to 0.2 m and low-amplitude flares resembling the flares of UV Ceti stars, but being more powerful and having longer durations. The variations of the stellar brightness are accompanied by variations of the B- V and V - R colors: when the brightness decreases, B- V decreases, while V - R increases (the star reddens). The reddening law is close to the standard interstellar reddening law. Although the character of the brightness variability ofMWC 297 resembles the photometric activity of UX Ori type stars, which is due to variations of their circumstellar extinction, its scale is very far from the scales observed for UX Ori stars. It is difficult to reconcile the level of photometric activity with the idea that MWC 297 is observed through its own gas-dust disk viewed almost edge-on, as has been suggested in several studies.

  7. KIC 8262223: A Post-mass Transfer Eclipsing Binary Consisting of a Delta Scuti Pulsator and a Helium White Dwarf Precursor

    Science.gov (United States)

    Guo, Zhao; Gies, Douglas R.; Matson, Rachel A.; García Hernández, Antonio; Han, Zhanwen; Chen, Xuefei

    2017-03-01

    KIC 8262223 is an eclipsing binary with a short orbital period (P = 1.61 day). The Kepler light curves are of Algol-type and display deep and partial eclipses, ellipsoidal variations, and pulsations of δ Scuti type. We analyzed the Kepler photometric data, complemented by phase-resolved spectra from the R-C Spectrograph on the 4 meter Mayall telescope at the Kitt Peak National Observatory and determined the fundamental parameters of this system. The low-mass and oversized secondary ({M}2=0.20{M}ȯ , {R}2=1.31{R}ȯ ) is the remnant of the donor star that transferred most of its mass to the gainer, and now the primary star. The current primary star is thus not a normal δ Scuti star but the result of mass accretion from a lower mass progenitor. We discuss the possible evolutionary history and demonstrate with the MESA evolution code that this system and several other systems discussed in prior literature can be understood as the result of non-conservative binary evolution for the formation of EL CVn-type binaries. The pulsations of the primary star can be explained as radial and non-radial pressure modes. The equilibrium models from single star evolutionary tracks can match the observed mass and radius ({M}1=1.94{M}ȯ , {R}1=1.67{R}ȯ ) but the predicted unstable modes associated with these models differ somewhat from those observed. We discuss the need for better theoretical understanding of such post-mass transfer δ Scuti pulsators.

  8. Obituary: James C. Kemp, 1927-1988

    Science.gov (United States)

    Milone, E. F.

    2009-01-01

    James C. Kemp was born in Detroit, Michigan on 9 February 1927, and died in Eugene, Oregon, on 29 March 1988. He went to high school in Mexico City and did undergraduate studies at the University of Michigan and University of California at Berkeley. Kemp was an active observational astronomer, having migrated from earlier interests in Slavic languages, in which he majored, electrical engineering, and physics. He obtained a PhD in electrical engineering at Berkeley in 1960 and did post-doctoral work there with Erwin Hahn on spin resonance. He went to the University of Oregon in 1961 and conducted research in magneto-optics, developing, in the process, a piezo-optical birefringence modulator to measure circular polarization. The modulator is described by Tinbergen (1996). Kemp explored new areas as he measured magnetic fields in the sunspots with polarized infrared light, and developed polarimeters and photometers to study the behavior of such astronomical sources as white dwarfs, the relativistic jets of binary SS 433, the x-ray binary Cyg X-1, and the bright eclipsing binaries Algol and e Aurigae on the 61- and, later, 81-cm telescope at the Pine Mountain Observatory, of which Kemp was director until his death from cancer. His measurement of circularly polarization in the continuum light of the white dwarf GJ 742 (Grw +70∘ 8247, Kemp et al. 1970b) was an important discovery, and through his study of Algol (Kemp et al. 1983; Wilson & Liou 1993), he appears to have been the first to discover the limb polarization in eclipsing binaries predicted by Chandrasekhar (1946ab). Although it has taken twenty years for the BAAS to publish his obituary notice, it is somewhat appropriate that his former student, Gary Henson, who provided much of the background for this article, is involved with a polarimetry team to observe and analyze data from e Aurigae, as it approaches ingress of the next primary minimum beginning summer, 2009. The author acknowledges with gratitude the

  9. Graeco-Roman Astro-Architecture: The Temples of Pompeii

    Science.gov (United States)

    Tiede, Vance R.

    2014-01-01

    Roman architect Marcus Vetruvius Pollio (ca. 75-15 BC) wrote, “[O]ne who professes himself as an architect should be…acquainted with astronomy and the theory of the heavens…. From astronomy we find the east, west, south, and north, as well as the theory of the heavens, the Equinox, Solstice and courses of the Stars.” (De Architectura Libri Decem I:i:3,10). In order to investigate the role of astronomy in temple orientation, the author conducted a preliminary GIS DEM/Satellite Imaging survey of 11 temples at Pompeii, Italy (N 40d 45', E 14d 29'). The GIS survey measured the true azimuth and horizon altitude of each temple’s major axis and was field checked by a Ground Truth survey with theodolite and GPS, 5-18 April 2013. The resulting 3D vector data was analyzed with Program STONEHENGE (Hawkins 1983, 328) to identify the local skyline declinations aligned with the temple major axes. Analysis suggests that the major axes of the temples of Apollo, Jupiter and Venus are equally as likely to have been oriented to Pompeii’s urban grid, itself oriented NW-SE on Mt. Vesuvius’ slope and hydraulic gradient to optimize urban sewer/street drainage (cf. Hodge 1992). However, the remaining nine temples appear to be oriented to astronomical targets on the local horizon associated with Graeco-Roman calendrics and mythology. TEMPLE/ DATE/ MAJOR AXIS ASTRO-TARGET (Skyline Declination in degrees) Public Lares/AD 50/ Cross-Quarter 7 Nov/3 Feb Sun Set, Last Gleam (-16.5) Vespsian/ AD 69-79/ Cross-Quarter 7 Nov/3 Feb Sun Set, LG (-16.2) Fortuna Augusta/ AD 1/ Winter Solstice Sun Set, LG (-22.9) Aesculapius/ 100 BC/ Perseus Rise (β Persei-Algol = +33.0) & Midsummer Moon Major Stand Still Set, LG (-28.1) Isis/ 100 BC/ Midwinter Moon Major Stand Still Rise, Tangent (+28.5) & Equinox Sun Set, Tangent (-0.3) Jupiter/ 150 BC/ Θ Scorpionis-Sargas Rise (-38.0) Apollo/ 550 (rebuilt 70 BC)/ α Columbae-Phact Rise (-37.1) Venus/ 150 BC (rebuilt 70 BC)/ α Columbae-Phact Rise (-37

  10. Exploring the Variable Sky with the Sloan Digital Sky Survey

    Energy Technology Data Exchange (ETDEWEB)

    Sesar, Branimir; Ivezic, Zeljko; Lupton, Robert H.; Juric, Mario; Gunn, James E.; Knapp, Gillian R.; Lee, Nathan De; Smith, J.Allyn; Miknaitis, Gajus; Lin, Huan; Tucker,

    2007-04-01

    We quantify the variability of faint unresolved optical sources using a catalog based on multiple SDSS imaging observations. The catalog covers SDSS Stripe 82, which lies along the celestial equator in the Southern Galactic Hemisphere (22h 24m < {alpha}{sub J2000} < 04h 08m, -1.27 < {delta}{sub J2000} < +1.27, {approx}290 deg{sup 2} ), and contains 58 million photometric observations in the SDSS ugriz system for 1.4 million unresolved sources that were observed at least 4 times in each of the gri bands (with a median of 10 observations obtained over {approx}5 years). In each photometric bandpass we compute various low-order lightcurve statistics such as root-mean-square scatter (rms), {chi}{sup 2} 2 per degree of freedom, skewness, minimum and maximum magnitude, and use them to select and study variable sources. We find that 2% of unresolved optical sources brighter than g = 20.5 appear variable at the 0.05 mag level (rms) simultaneously in the g and r bands. The majority (2/3) of these variable sources are low-redshift (< 2) quasars, although they represent only 2% of all sources in the adopted ux-limited sample. We find that at least 90% of quasars are variable at the 0.03 mag level (rms) and confirm that variability is as good a method for finding low-redshift quasars as is the UV excess color selection (at high Galactic latitudes). We analyze the distribution of lightcurve skewness for quasars and find that is centered on zero. We find that about 1/4 of the variable stars are RR Lyrae stars, and that only 0.5% of stars from the main stellar locus are variable at the 0.05 mag level. The distribution of lightcurve skewness in the g-r vs. u-g color-color diagram on the main stellar locus is found to be bimodal (with one mode consistent with Algol-like behavior). Using over six hundred RR Lyrae stars, we demonstrate rich halo substructure out to distances of 100 kpc. We extrapolate these results to expected performance by the Large Synoptic Survey Telescope and

  11. Exploring the Variable Sky with the Sloan Digital Sky Survey

    Energy Technology Data Exchange (ETDEWEB)

    Sesar, Branimir; Ivezic, Zeljko; Lupton, Robert; Juric, Mario; Gunn, James; Knapp, Gillian; De Lee, Nathan; Smith, J. Allyn; Miknaitis,Gajus; Lin, Huan; Tucker, Douglas; Doi, Mamoru; Tanaka, Masayuki; Fukugita, Masataka; Holtzman, Jon; Kent, Steve; Yanny, Brian; Schlegel,David; Finkbeiner, Douglas; Padmanabhan, Nikhil; Rockosi, Constance; Bond, Nicholas; Lee, Brian; Stoughton, Chris; Jester, Sebastian; Harris,Hugh; Harding, Paul; Brinkmann, Jon; Schneider, Donald; York, Donald; Richmond, Michael; Vanden Berk, Daniel

    2007-04-01

    We quantify the variability of faint unresolved optical sources using a catalog based on multiple SDSS imaging observations. The catalog covers SDSS Stripe 82, which lies along the celestial equator in the Southern Galactic Hemisphere (22h 24m < {alpha}{sub J2000} < 04h 08m, -1.27{sup o} < {delta}{sub J2000} < +1.27{sup o}, {approx} 290 deg{sup 2}), and contains 58 million photometric observations in the SDSS ugriz system for 1.4 million unresolved sources that were observed at least 4 times in each of the gri bands (with a median of 10 observations obtained over {approx}5 years). In each photometric bandpass we compute various low-order lightcurve statistics such as root-mean-square scatter (rms), {chi}{sup 2} per degree of freedom, skewness, minimum and maximum magnitude, and use them to select and study variable sources. We find that 2% of unresolved optical sources brighter than g = 20.5 appear variable at the 0.05 mag level (rms) simultaneously in the g and r bands. The majority (2/3) of these variable sources are low-redshift (< 2) quasars, although they represent only 2% of all sources in the adopted flux-limited sample. We find that at least 90% of quasars are variable at the 0.03 mag level (rms) and confirm that variability is as good a method for finding low-redshift quasars as is the UV excess color selection (at high Galactic latitudes). We analyze the distribution of lightcurve skewness for quasars and find that is centered on zero. We find that about 1/4 of the variable stars are RR Lyrae stars, and that only 0.5% of stars from the main stellar locus are variable at the 0.05 mag level. The distribution of lightcurve skewness in the g-r vs. u-g color-color diagram on the main stellar locus is found to be bimodal (with one mode consistent with Algol-like behavior). Using over six hundred RR Lyrae stars, we demonstrate rich halo substructure out to distances of 100 kpc. We extrapolate these results to expected performance by the Large Synoptic Survey

  12. VizieR Online Data Catalog: JMMC Stellar Diameters Catalogue - JSDC. Version 2 (Bourges+, 2017)

    Science.gov (United States)

    Bourges, L.; Mella, G.; Lafrasse, S.; Duvert, G.; Chelli, A.; Le Bouquin, J.-B.; Delfosse, X.; Chesneau, O.

    2017-01-01

    The JMMC (Jean-Marie Mariotti Center) Calibrator Workgroup has long developed methods to estimate the angular diameter of stars, and provides this expertise in the SearchCal tool (http://www.jmmc.fr/searchcal). SearchCal creates a dynamical catalogue of stars suitable to calibrate Optical Long-Baseline Interferometry (OLBI) observations from on-line queries of CDS catalogues, according to observational parameters. In essence, SearchCal is limited only by the completeness of the stellar catalogues it uses, and in particular is not limited in magnitude. SearchCal being an application centered on the somewhat restricted OLBI observational purposes, it appeared useful to make our angular diameter estimates available for other purposes through a CDS-based catalog, the JMMC Stellar Diameters Catalogue (JSDC, II/300). This second version of the catalog represents a tenfold improvement both in terms of the number of objects and on the precision of the estimates. This is due to a new algorithm using reddening-free quantities -- the pseudomagnitudes, allied to a new database of all the measured stellar angular diameters -- the JMDC (II/345/jmdc), and a rigorous error propagation at all steps of the processing. All this is described in the associated publication by Chelli et al. (2016A&A...589A.112C). The catalog reports the Limb-Darkened Diameter (LDD) and error for 465877 stars, as well as their BVRIJHKLMN magnitudes, Uniform Disk Diameters (UDD) in these same photometric bands, Spectral Type, and two supplementary quality indicators: - the mean-diameter chi-square (see Appendix A.2 of Chelli et al., 2016A&A...589A.112C). - a flag indicating some degree of caution in choosing this star as an OLBI calibrator: known spectroscopic binaries, Algol type stars, etc, see Note (1). The conversion from LDD to UDD in each spectral band is made using mainly the coefficients from J/A+A/556/A86/table16 and J/A+A/554/A98/table16 when possible (compatible spectral types) and following the

  13. Large X-ray flares on stars detected with MAXI/GSC: A universal correlation between the duration of a flare and its X-ray luminosity

    Science.gov (United States)

    Tsuboi, Yohko; Yamazaki, Kyohei; Sugawara, Yasuharu; Kawagoe, Atsushi; Kaneto, Soichiro; Iizuka, Ryo; Matsumura, Takanori; Nakahira, Satoshi; Higa, Masaya; Matsuoka, Masaru; Sugizaki, Mutsumi; Ueda, Yoshihiro; Kawai, Nobuyuki; Morii, Mikio; Serino, Motoko; Mihara, Tatehiro; Tomida, Hiroshi; Ueno, Shiro; Negoro, Hitoshi; Daikyuji, Arata; Ebisawa, Ken; Eguchi, Satoshi; Hiroi, Kazuo; Ishikawa, Masaki; Isobe, Naoki; Kawasaki, Kazuyoshi; Kimura, Masashi; Kitayama, Hiroki; Kohama, Mitsuhiro; Kotani, Taro; Nakagawa, Yujin E.; Nakajima, Motoki; Ozawa, Hiroshi; Shidatsu, Megumi; Sootome, Tetsuya; Sugimori, Kousuke; Suwa, Fumitoshi; Tsunemi, Hiroshi; Usui, Ryuichi; Yamamoto, Takayuki; Yamaoka, Kazutaka; Yoshida, Atsumasa

    2016-10-01

    Twenty-three giant flares from thirteen active stars (eight RS CVn systems, one Algol system, three dMe stars, and one young stellar object) were detected during the first two years of our all-sky X-ray monitoring with the gas propotional counters (GSC) of the Monitor of All-sky X-ray Image (MAXI). The observed parameters of all these MAXI/GSC flares are found to be at the upper ends for stellar flares with the luminosity of 1031-34 erg s-1 in the 2-20 keV band, the emission measure of 1054-57 cm-3, the e-folding time of 1 hr to 1.5 d, and the total radiative energy released during the flare of 1034-39 erg. Notably, the peak X-ray luminosity of 5^{+4}_{-2} × 10^{33}erg s-1 in the 2-20 keV band was detected in one of the flares on II Peg, which is one of the, or potentially the, largest-ever-observed in stellar flares. X-ray flares were detected from GT Mus, V841 Cen, SZ Psc, and TWA-7 for the first time in this survey. Whereas most of our detected sources are multiple-star systems, two of them are single stars (YZ CMi and TWA-7). Among the stellar sources within 100 pc distance, the MAXI/GSC sources have larger rotation velocities than the other sources. This suggests that the rapid rotation velocity may play a key role in generating large flares. Combining the X-ray flare data of nearby stars and the sun, taken from literature and our own data, we discovered a universal correlation of τ ∝ L_X^{0.2} for the flare duration τ and the intrinsic X-ray luminosity LX in the 0.1-100 keV band, which holds for 5 and 12 orders of magnitude in τ and LX, respectively. The MAXI/GSC sample is located at the highest ends of the correlation.

  14. The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

    Science.gov (United States)

    Kim, Hyoun-Woo; Kim, Chun-Hwey; Song, Mi-Hwa; Jeong, Min-Ji; Kim, Hye-Young

    2016-09-01

    New multiband BVRI light curves of NSVS 1461538 were obtained as a byproduct during the photometric observations of our program star PV Cas for three years from 2011 to 2013. The light curves indicate characteristics of a typical W-subtype W UMa eclipsing system, displaying a flat bottom at primary eclipse and the O’Connell effect, rather than those of an Algol/ b Lyrae eclipsing variable classified by the northern sky variability survey (NSVS). A total of 35 times of minimum lights were determined from our observations (20 timings) and the SuperWASP measurements (15 ones). A period study with all the timings shows that the orbital period may vary in a sinusoidal manner with a period of about 5.6 yr and a small semiamplitude of about 0.008 day. The cyclical period variation can be interpreted as a light-time effect due to a tertiary body with a minimum mass of 0.71 M⊙. Simultaneous analysis of the multiband light curves using the 2003 version of the WilsonDevinney binary model shows that NSVS 1461538 is a genuine W-subtype W UMa contact binary with the hotter primary component being less massive and the system shows a low mass ratio of q(mc/mh)=3.51, a high orbital inclination of 88.7°, a moderate fill-out factor of 30 %, and a temperature difference of ΔT=412 K. The O’Connell effect can be similarly explained by cool spots on either the hotter primary star or the cool secondary star. A small third-light corresponding to about 5 % and 2 % of the total systemic light in the B and V bandpasses, respectively, supports the third-body hypothesis proposed by the period study. Preliminary absolute dimensions of the system were derived and used to look into its evolutionary status with other W UMa binaries in the mass-radius and mass-luminosity diagrams. A possible evolution scenario of the system was also discussed in the context of the mass vs mass ratio diagram.

  15. High-dispersion spectroscopy of two A supergiant systems in the Small Magellanic Cloud with novel properties

    Science.gov (United States)

    Mennickent, R. E.; Smith, M. A.

    2010-09-01

    We present the results of a spectroscopic investigation of two novel variable bright blue stars in the SMC, OGLE004336.91-732637.7 (SMC-SC3) and the periodically occulted star OGLE004633.76-731204.3 (SMC-SC4), whose photometric properties were reported by Mennickent et al. (2010). High-resolution spectra in the optical and far-UV show that both objects are actually A + B type binaries. Three spectra of SMC-SC4 show radial velocity variations, consistent with the photometric period of 184.26 d found in Mennickent et al. 2010. The optical spectra of the metallic lines in both systems show combined absorption and emission components that imply that they are formed in a flattened envelope. A comparison of the radial velocity variations in SMC-SC4 and the separation of the V and R emission components in the Hα emission profile indicate that this envelope, and probably also the envelope around SMC-SC3, is a circumbinary disc with a characteristic orbital radius some three times the radius of the binary system. The optical spectra of SMC-SC3 and SMC-SC4 show, respectively, HeI emission lines and discrete blue absorption components (BACs) in metallic lines. The high excitations of the HeI lines in the SMC-SC3 spectrum and the complicated variations of FeII emission and absorption components with orbital phase in the spectrum of SMC-SC4 suggests that shocks occur between the winds and various static regions of the stars' corotating binary-disc complexes. We suggest that BACs arise from wind shocks from the A star impacting the circumbinary disc and a stream of former wind-efflux from the B star accreting on to the A star. The latter picture is broadly similar to mass transfer occurring in the more evolved (but less massive) ALGOL (B/A + K) systems, except that we envision transfer occurring in the other direction and not through the inner Lagrangian point. Accordingly, we dub these objects prototype of a small group of Magellanic Cloud wind-interacting A + B binaries.

  16. Photometric activity of UX Ori stars and related objects in the near infrared and visual. BF Ori, CQ Tau, WW Vul, and SV Cep

    Science.gov (United States)

    Shenavrin, V. I.; Grinin, V. P.; Rostopchina-Shakhovskaja, A. N.; Demidova, T. V.; Shakhovskoi, D. N.

    2012-05-01

    We have analyzed the activity of four UX Ori stars in the near-IR ( JHKL) and visual ( V) using the results of long-term photometric observations. For comparison, we also obtained IR ( JHKLM) photometric observations of two visually quiet young stars of close spectral types (AB Aur and HD 190073). For the photometrically most active UX Ori stars BF Ori, CQ Tau, and WW Vul, the Algol-like declines of brightness in the visual, which are due to sporadic enhancements of the circumstellar extinction, are also observed (with decreasing amplitude) in the IR bands. A strict correlation between the V and J brightness variations is observed for all the stars except for SV Cep. For some of the UX Ori stars, a strong correlation between the visual and IR activity is observed up to L, where the main contribution to the emission is made by circumstellar dust. In the case of SV Cep, the visual variability is not correlated with the variability of the IR fluxes. On one occasion, a clear anti-correlation was even observed: a shallow, but prolonged decrease of the visual brightness was accompanied by an increase in the IR fluxes. This indicates that circumstellar clouds themselves can become powerful sources of IR emission. Our results provide evidence that the photometric activity of UX Ori stars is a consequence of instability of the deepest layers of their gas-dust accretion disks. In some cases (SV Cep), fluctuations of the density in this region are global, in the sense that they occur along a significant part of the circle marking the inner boundary of the dust disk. It is interesting that AB Aur, which is the quietest in the visual, appeared to be the most active in the IR. In contrast to UX Ori stars, the amplitude of its brightness variations increases from the J to the M band. It follows from analysis of the IR colors of this star that their variability cannot be described by models in which the variable IR emission has a temperature close to the sublimation temperature of

  17. Implications of the Turing machine model of computation for processor and programming language design

    Science.gov (United States)

    Hunter, Geoffrey

    2004-01-01

    ; it may be allocated as its execution commences, and deallocated as its execution terminates, and if the amount of this local memory is not known until just before execution commencement, then it is essential that it be allocated dynamically as the first action of its execution. This dynamically allocated/deallocated storage of each subprogram"s intermediate values, conforms with the stack discipline; i.e. last allocated = first to be deallocated, an incidental benefit of which is automatic overlaying of variables. This stack-based dynamic memory allocation was a semantic implication of the nested block structure that originated in the ALGOL-60 programming language. AGLOL-60 was a TM language, because the amount of memory allocated on subprogram (block/procedure) entry (for arrays, etc) was computable at execution time. A more general requirement of a Turing machine process is for code generation at run-time; this mandates access to the source language processor (compiler/interpretor) during execution of the process. This fundamental aspect of computer science is important to the future of system design, because it has been overlooked throughout the 55 years since modern computing began in 1048. The popular computer systems of this first half-century of computing were constrained by compile-time (or even operating system boot-time) memory allocation, and were thus limited to executing FA processes. The practical effect was that the distinction between the data-invariant program and its variable data was blurred; programmers had to make trial and error executions, modifying the program"s compile-time constants (array dimensions) to iterate towards the values required at run-time by the data being processed. This era of trial and error computing still persists; it pervades the culture of current (2003) computing practice.

  18. Light curve solutions and study of roles of magnetic fields in period variations of the UV Leo system

    Directory of Open Access Journals (Sweden)

    D Manzoori

    2009-12-01

    Full Text Available The solutions of photometric BV light curves for the Algol like system UV Leo were obtained using Wilson-Devinney code. The physical and orbital parameters along with absolute dimensions of the system were determined. It has been found that to best fit the V light curve of the system, assumptions of three dark spots were necessary two on the secondary and one on the primary. The absolute visual magnitudes (Mv of the individual components i.e., primary and secondary were estimated to 4.41 and 4.43, respectively, through the color curve analysis. The period analysis of the system presented elsewhere, indicated a cyclic period change of 12 yr duration, which was attributed to magnetic activity cycle, as a main cause of period variation in the system, through the Applegate mechanism. To verify the Applegate model I preformed calculations of some related parameters barrowed from Apllegate and Kalimeris. Values of all the calculated parameters were in accordance to those obtained for similar systems by Applegate. The differential magnitudes Δ B and Δ V, along with corresponding values of Δ(B-V color index. The cyclic variations in brightness are quite clear. There are three predictions of Applegate's theory concerning effects of cyclic magnetic changes on the period variations, which can be checked through the observations, these are as follows: I The long term variations in mean brightness (at outside of eclipses and cyclic changes of orbital period, vary with the same period. II The active star gets bluer as it gets brightened and/or the brightness and color variations are to be in phase. III Changes in luminosity due to changes in quadrupole moment should be of the order 0.1 mag. All the above mentioned predictions of Applegate’s theory are verified. These results combined with cyclic character of P(E presented elsewhere and also consistency of parameters which are obtained in this paper, led me to conclude that one the main causes of period

  19. 云南天文台2000年度学术论文汇总

    Institute of Scientific and Technical Information of China (English)

    2001-01-01

    @@一、发表论文 1、 SCI(科学引文索引)类论文 1) 一个日珥D3线的特征和计算=Calculations and physical properties of the D3 emission lines of a prominence.李可军,顾啸马,陈学昆.MNRAS,2000,Vol.313,761-766. 2) 两个相接双星TZ Boo和Y Sex的轨道周期研究=Orbital period Studies of the two contact binaries TZ Bootis and Y Sextantis.钱声邦,刘清耀.A&A,2000,Vol.355,171-175. 3) 1998年在云南的狮子座流星雨目视观测=Visual observations of the leonid meteors 1998 in Yunnan.吴光节,张周生.Earth,Moon,and Planets,2000,Vol.81,No.3,193-200. 4) 微波弱偏振尖峰的观测特征=Observational characteristics of weak polarized microwave spikes.汪敏,傅其骏,谢瑞祥,黄光力.Solar Physics,1999,Vol.189,331-344. 5) 重联对日冕物质抛射过程的影响=Effects of reconnection on the coronal mass ejection process.林隽,Forbes T.G. Journal of Geophysical Research ,2000,Vol.105,No.A2,2375-2392. 6) 正至冷却的相对论电子模拟=Simulation of Gamma-Ray bursts from cooling relativistic electrons.王建成,岑学奋,钱铜铃,许骏,汪从云.ApJ,2000,Vol.532,267-272. 7) 非同步转动双星系统的演化=Evolution of non-synchronized binary systems.黄润乾,曾艺蓉.中国科学(A辑),2000,Vol.30,No.2,187. 8) 21周太阳活动真的是南占优吗?=Does the southern dominance of solar activity really exist in solar cycle 21.李可军,顾啸马.A&A,2000,Vol.353,396. 9) 湍流对太阳P-模振荡的影响=The influence of turbulence on the solar P-mode oscillations.毕少兰,许华 .A&A,2000,Vol.357,330-336. 10) Algol型双星可能的质量和角动量损失=Possible mass and angular momentum loss in Algol-type binaries.II TT Del Bo Mon and Y Psc.钱声邦.AJ,2000,Vol.119,3064.

  20. BOOK REVIEW: Numerical Recipes in C++: The Art of Scientific Computing (2nd edn)1 Numerical Recipes Example Book (C++) (2nd edn)2 Numerical Recipes Multi-Language Code CD ROM with LINUX or UNIX Single-Screen License Revised Version3Numerical Recipes in C++: The Art of Scientific Computing (2nd edn) Numerical Recipes Example Book (C++) (2nd edn) Numerical Recipes Multi-Language Code CD ROM with LINUX or UNIX Single-Screen License Revised Version

    Science.gov (United States)

    Press, William H.; Teukolsky, Saul A.; Vettering, William T.; Flannery, Brian P.

    2003-05-01

    (C++), the authors point out some of the problems in the use of C++ in scientific computing. I have not found any mention of parallel computing in NR(C++). Fortran has quite a lot going for it. As someone who has used it in most of its versions from Fortran II, I have seen it develop and leave behind other languages promoted by various enthusiasts: who now uses Algol or Pascal? I think it unlikely that C++ will disappear: it was devised as a systems language, and can also be used for other purposes such as scientific computing. It is possible that Fortran will disappear, but Fortran has the strengths that it can develop, that there are extensive Fortran subroutine libraries, and that it has been developed for parallel computing. To argue with programmers as to which is the best language to use is sterile. If you wish to use C++, then buy NR(C++), but you should also look at volume 2 of NR(F). If you are a Fortran programmer, then make sure you have NR(F), volumes 1 and 2. But whichever language you use, make sure you have one version or the other, and the CD ROM. The Example Book provides listings of complete programs to run nearly all the routines in NR, frequently based on cases where an anlytical solution is available. It is helpful when developing a new program incorporating an unfamiliar routine to see that routine actually working, and this is what the programs in the Example Book achieve. I started teaching computational physics before Numerical Recipes was published. If I were starting again, I would make heavy use of both The Art of Scientific Computing and of the Example Book. Every computational physics teaching laboratory should have both volumes: the programs in the Example Book are included on the CD ROM, but the extra commentary in the book itself is of considerable value. P Borcherds