Catalogue of Ap, HgMn and Am stars
We present a catalogue of 8205 known or suspected Ap, HgMn and Am stars.This paper is a major update of our first edition of the catalog of Apand Am stars and includes revised identifications, additional stars andrevised information obtained from the literature.Catalogue (full Table 1) is only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/498/961
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B.R.N.O. Contributions #34
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Photoelectric Minima of Selected Eclipsing Binaries and Maxima of Pulsating Stars
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CCD Minima for Selected Eclipsing Binaries in 2007
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Photoelectric Minima of Selected Eclipsing Binaries and Maxima of Pulsating Stars
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A catalogue of eclipsing variables
A new catalogue of 6330 eclipsing variable stars is presented. Thecatalogue was developed from the General Catalogue of Variable Stars(GCVS) and its textual remarks by including recently publishedinformation about classification of 843 systems and making correspondingcorrections of GCVS data. The catalogue1 represents thelargest list of eclipsing binaries classified from observations.
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Beobachtungssergebnisse Bundesdeutsche Arbeitsgemeinschaft fuer Veraenderliche Sterne e.V.
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163. List of Minima Timings of Eclipsing Binaries by BBSAG Observers
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Up-to-Date Linear Elements of Eclipsing Binaries
About 1800 O-C diagrams of eclipsing binaries were analyzed and up-todate linear elements were computed. The regularly updated ephemerides(as a continuation of SAC) are available only in electronic form at theInternet address: http://www.as.ap.krakow.pl/ephem/.
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CCD Minima for Selected Eclipsing Binaries in 2003
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Beobachtungsegebnisse Bundesdeutsche Arbeitsgemainschaft fur Veranderliche Sterne e.V.
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CCD Times of Minima of Faint Eclipsing Binaries in 2000
196 CCD minima observations of 122 eclipsing binaries made by the authorin 2000 are presented. The observed stars were chosen from the catalogueBRKA of observing programme of BRNO-Variable Star Section of CAS.
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CCD Times of Minima of Faint Eclipsing Binaries III
We present 248 CCD minima observations of 170 eclipsing binaries made in1999. The observed stars were chosen from catalogue BRKA of observingprogramme of BRNO-Variable Star Section of CAS.
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Minima of binary stars
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149 Bedeckungssterne der BAV-Programme. Eine Analyse der Beobachtungstatigkeit seit den Angangen.
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Das Brunner Punktesystem.
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Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
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The observed periods of AP and BP stars
A catalogue of all the periods up to now proposed for the variations ofCP2, CP3, and CP4 stars is presented. The main identifiers (HD and HR),the proper name, the variable-star name, and the spectral type andpeculiarity are given for each star as far as the coordinates at 2000.0and the visual magnitude. The nature of the observed variations (light,spectrum, magnetic field, etc.) is presented in a codified way. Thecatalogue is arranged in three tables: the bulk of the data, i.e. thosereferring to CP2, CP3, and CP4 stars, are given in Table 1, while thedata concerning He-strong stars are given in Table 2 and those foreclipsing or ellipsoidal variables are collected in Table 3. Notes arealso provided at the end of each table, mainly about duplicities. Thecatalogue contains data on 364 CP stars and is updated to 1996, October31. This research has made use of the SIMBAD database, operated at CDS,Strasbourg, France.
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Photoelectric Minima of Selected Eclipsing Binaries
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Four-Colour Photometry of Eclipsing Binaries - Part Twenty-Seven - a Photometric Analysis of the Possible Ap-System Ao-Velorum
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995A&AS..109..425C&db_key=AST
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Four short-period ALGOLS
The light curves of four close binary star systems (BV 267, RU UMi, XZCMi, and VV UMa) have been analyzed using the Wilson-Devinneydifferential corrections model. The present system geometries of thesebinaries is that of short-period semi-detached systems withRoche-lobe-filling secondaries and main-sequence primaries. Differentialcoordinates in the mass-luminosity and mass-radius diagrams indicatethat the secondary components lie near the main sequence, except in thecase of BV 267. It is suggested that these systems are binaries withslightly overluminous and oversized secondaries which have undergonecase A mass transfer. This contention is supported by timinginformation, and qualitatively by the period-frequency relation. Thesevery-nearly contact binaries are likely candidates for postcontactsystem evolution.
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Statistical study of semi-detached and near-contact semi-detached binaries
A statistical study was made of 107 semidetached with combined lightcurve solutions. An empirical period-dependent mass-radius relation wasderived, thereby revealing the impossibility of having evolvedsemidetached systems with very short periods. Statistically, thenear-contact semidetached systems have the common properties of nearlyequal mass densities of the components, larger mass-ratios, shorterperiods and smaller specific angular momenta, and their A- F-typesecondaries generally have greater densities than the secondaries ofclassical Algol systems of the same spectral types. A detaileddiscussion is also made in this paper on the evolution of near-contactsemidetached binaries.
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Statistical Study on the Semidetached and Near Contact Semidetached Binary Systems
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First supplement to the catalog of observed periods of AP stars
Supplementary data on the periods of Ap stars with references arepresented; 58 new stars are introduced for which periodic variabilityhas been discovered since 1983. For some of these stars periodicity wasknown before 1983 but they were not reported in the previous catalog.Recently attributed variable star names are also reported.
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Photoelectric observations of AX Virginis and a photometric solution
A photoelectric light curve of AX Virginis has been obtained based on686 single observations in yellow light. The outside eclipse light curvewas fitted with a finite Fourier series, and the least squares solutionfor the coefficient and their probable errors are shown. The shape ofthe curve inside eclipses indicates that the eclipses are partial. TheRussell-Merrill method is used to solve for the orbital elements. Theresults show that the stars strongly depart from the similar, rotationalellipsoids assumed in the method, and that the darker (due to gravitydarkening) component is much more distorted than the brighter one.
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Two almost-contact semidetached systems - ZZ Aurigae and AX Virginis
Photoelectric observations of ZZ Aur and AX Vir from Yunnan and Beijingobservatories were analyzed by the Wilson-Devinney method. The systemsare very similar to each other, and appropriate values of their massratios were obtained. A semidetached configuration exists where thelower-mass components are in contact with their respective Rochesurface, and both of the higher-mass components very nearly fill theirRoche lobes. It is shown that these systems are very close to being acritical contact configuration, and ZZ Aur and AX Vir are extremelysimilar to the semidetached SX Aur. It is concluded that the lower-mass(contact) component is the loser during the mass-loss phase ofevolution, while the gainer (more massive component) has recently becomedetached from its Roche surface. It is suggested that a system of thistype is at an evolutionary stage.
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Une autre etoile Ap a eclipses?
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Analysis of 11 Late-Type Close Binary Systems
This is a preliminary report on the joint research project between 3observatories: Beijing, Yunnan, and Behlen Observatories from China andthe United States. The systems we have been dealing with are primary oflate spectral types and with short periods. Most of the observationswere secured from the observatories in China. The computational analysisis carried out in University of Nebraska, Lincoln. The photometricsolutions are based on the Wilson and Devinney method. Out of 11 systemsanalyzed 6 of them: AO Cam, ER Ori. BX Peg, BB Peg, U Peg, and SW Lacare found to be contact systems. All of them are having their primaryeclipses at occultation. Therefore they can be classified as W-type W UMa systems. They also show other W-type characteristics. Three systems:ZZ Aur, RZ Dra, and AX Vir are found to be semi-detached systems, withlow mass components filling their Roche surfaces. The massive componentsare having their radii fairly close to Roche surfaces and are largerthan their contact companions. The last two systems: AT Cam and AZ Camare found to be detached systems, but with their low mass componentsalmost filling their Roche surfaces. This type of configuration is ofgreat interest to our understanding of close binary evolution. Webelieve that these systems are at phase immediately after the normalAlgol phase, where the mass lossing components detached from the Rochesurfaces at the conclusion active mass lost phase.
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Statistics of categorized eclipsing binary systems Lightcurve shapes, periods, and spectral types
The statistics of the light curve morphologies, eclipse depths, orbitalperiods, and spectral types of about 1000 eclipsing binary systems areexamined, after attempting to subdivide these binaries into variousbasic evolutionary categories. The applicability of statisticalcriteria, based on light curve morphologies and eclipse depths, for thecategorization of eclipsing binaries has been found more limited thanpreviously believed. In particular, EW-type light curves turn out to begood indicators of contact systems (though not conversely), while EA-and EB-type light curves have little physical significance. Moreover,the study reveals a strong deficit of short-period noncontact systems inthe whole spectral range, together with an underabundance of early-typecontact binaries (compared with the number of late-type contact pairs).Interestingly, the distribution of evolved Algol-type systems isshifted, on average, to periods longer than those of unevolved detachedsystems in the OB and early A spectral range (and to shorter periods inthe F spectral range).
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Analysis of eleven late-type close binary systems.
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