Radial Velocity Studies of Southern Close Binary Stars. II. Spring/Summer Systems
Radial velocity measurements and sine-curve fits to the orbital velocityvariations are presented for 14 close binary stars, S Ant, TT Cet, TWCet, AA Cet, RW Dor, UX Eri, YY Eri, BV Eri, CT Eri, SZ Hor, AD Phe, TYPup, HI Pup, and TZ Pyx. All are double-lined binaries, and all exceptthe last one are contact binaries. The orbital data must be consideredpreliminary because of the relatively small number of observations(6-12), a circumstance that is partly compensated by the good definitionof the broadening functions used for the radial velocity determinations.Based on data obtained at the European Southern Observatory.
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Variation in the orbital period of W UMa-type contact systems
The secular variation in the orbital period Porb is studiedas a function of the mass ratio q of the components in a sample of 73contact systems of class W UMa constructed from a survey of current(1991–2003) published photometric and spectroscopic data. Almostall the W UMa-systems (>93% of this sample) are found to have avariation in their orbital periods Porb which alternates insign independently of their division into A-and Wsubclasses. Astatistical study of this sample in terms of the observedcharacteristics dPorb/dt and q showed that on the average thenumbers of increases (35 systems) and decreases (33 systems) in theperiods are the same, which indicates the existence of flows directedalternately from one component to the other and illustrates the cyclicalcharacter of the thermal oscillations. An analysis of the behavior ofdPorb/dt as a function of the mass interval of the primarycomponent yields a more accurate value for the mass ratio, q ≈ 0.4÷ 0.45 at which contact binaries are separated into A-andW-subclasses. No correlations were observed between the fill-out factorfor the outer contact configuration, the total mass of the contactsystem, and the mass ratio of the components, on one hand, and the signof the secular variation in the period. The physical properties andevolutionary features of these systems are discussed.
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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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SB9: The ninth catalogue of spectroscopic binary orbits
The Ninth Catalogue of Spectroscopic Binary Orbits(http://sb9.astro.ulb.ac.be) continues the series of compilations ofspectroscopic orbits carried out over the past 35 years by Batten andcollaborators. As of 2004 May 1st, the new Catalogue holds orbits for2386 systems. Some essential differences between this catalogue and itspredecessors are outlined and three straightforward applications arepresented: (1) completeness assessment: period distribution of SB1s andSB2s; (2) shortest periods across the H-R diagram; (3)period-eccentricity relation.
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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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Period Changes of Two W UMa-Type Contact Binaries: RW Comae Berenices and CC Comae Berenices
From the present times of minimum light and those collected from theliterature, changes in the orbital period of the two W UMa-type contactbinaries RW Com and CC Com are analyzed. The results reveal that theperiod changes of these two systems show the same natures, with ashort-term oscillation superposed on the secular decrease. For RW Com,its period shows a secular decrease at a rate ofdP/dt=0.43×10-7 days yr-1. An oscillationwith a periodicity of 13.7 yr and an amplitude ofΔP=5.4×10-7 days is superposed on the seculardecrease. For CC Com, its period shows a secular decrease at a rate ofdP/dt=0.40×10-7 days yr-1. An oscillationwith a periodicity of 16.1 yr and an amplitude ofΔP=2.8×10-7 days is superposed on the seculardecrease. The period secular decreases of the two systems may beexplained by a mass-transfer rate of dm/dt=0.29×10-7Msolar yr-1 for RW Com anddm/dt=0.52×10-7 Msolar yr-1 forCC Com. The period short-term oscillations of the two systems may beexplained by the magnetic activity cycle model given by Applegate, andthe parameters for the magnetic activity cycle model are presented.
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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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Period changes in W UMa-type eclipsing binaries: DK Cygni, V401 Cygni, AD Phoenicis and Y Sextantis
We present a period analysis of the four well-known W UMa-type eclipsingbinaries DK Cyg (P = 0fd47 ), V401 Cyg (0fd58 ), AD Phe (0fd38 ) and YSex (0fd42 ). Several new times of minimum light, recordedphotoelectrically, have been gathered. Analysis of all available eclipsetimings of the DK Cygni and V401 Cygni has confirmed a significantincrease in period of 1.15 10-10 and 1.48 10-10day cycle-1, respectively. A simultaneous solution of the B,V and R light curves was computed for V401 Cyg using the Binary Maker2.0 synthetic lightcurve software. This solution indicates that V401 Cygis in contact with a filing factor of 46%. The period of AD Phe seems tobe constant. Period changes of Y Sex could be explain by a light-timeeffect caused by a third body in an eccentric orbit with a period of 58years. Some of the observations reported in this paper were obtained atthe South Africa Astronomical Observatory, Sutherland, South Africa.
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CCD photometry and astrometry of visual double and multiple stars of the HIPPARCOS Catalogue. II. CCD photometry and differential astrometry of 288 southern ``Intermediate'' systems
We present photometric and astrometric data of about 280 visual doublestars of the ``intermediate'' class, i.e. with angular separationsmainly in the range 2arcsec < rho < 12arcsec . The observationshave been obtained in 1991-92 with a CCD camera attached to the 91 cmDutch telescope at ESO La Silla, Chile. Differential magnitudes of thedouble star components as well as magnitudes and colour indices of theindividual components have been determined in the Cousins V and Ipassbands with an internal error of about 0.005 mag and an externalaccuracy of less than 0.03 mag. In addition, angular separations havebeen secured to an internal accuracy of 0.004arcsec and position anglesto about 0.05degr. Tables 1 to 4 are only available in electronic format the CDS via ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html. Based on observationscollected at the European Southern Observatory, La Silla, Chile.
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A note on thermally decoupled W Ursae Majoris systems
The thermal decoupling degree of short-period contact or near-contactsystems is studied. Statistics of well-observed W UMa systems includingnew beta-light-curve objects was made for thermal-decoupling degree,spectral type, and orbital period. W UMa systems of type A and W arefound to be well characterized by these parameters. W-type objects showa good (linear) correlation in the spectral type vs. thermal-decouplingparameter diagram. This extends to the lower border of the diagram forA-type systems, otherwise scattered in an area of large thermaldecoupling. These empirical facts are analyzed in terms of contact ornoncontact configurations.
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Studies of Period Variation in Close Binary Systems
Abstract image available at:http://adsabs.harvard.edu/abs/1987AJ.....94..792L
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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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Violet and ultraviolet continua of W UMa systems on the basis of UVBY photometry observations
New observations of 17 southern WUMa systems are discussed together withprevious uvby data for 44 systems to determine properties of violet andultraviolet spectral distributions and to relate them to theperiod-color relation. The interstellar-reddening-corrected delta(m1)values extend from -0.02 to +0.10, which could be interpreted by aplausible range of metallicities; the most positive values of delta(m1)and largest ultraviolet excesses are observed for systems having theshortest periods at a given spectral type. The reddening-correcteddelta(c1) values are close to zero and are only slightly positive forearlier spectral types - mean delta (cl) = +0.04 for (b-y)O less than0.31 - indicating only very slight evolutionary advancement. Traces of adelta(cl) = -delta(ml) correlation for least evolved systems - smallestdelta(cl) - leave the possibility of intrinsic excesses still open.
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A uvby, beta photometric survey of southern hemisphere
A uvby, beta photometric study of southern hemisphere eclipsing binarystars has been undertaken at Cerro Tololo Inter-American Observatory.The standardized colors and V magnitudes for 288 binaries at quadratureand/or at minimum are presented, along with an indication of theaccuracy of the standardization and photometry. Discussions of theresolving time of the pulse-counting photometers and of the atmosphericextinction at CTIO are included.
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BV DRA and BW DRA - Two contact systems in one visual binary
UBV light curves obtained in 1975 for both components of ADS 9537, aswell as Yamasaki's (1979) light curve for BV Dra, are solved forgeometrical parameters using the synthesis method under two hypotheseswhich explain the W-subclass light curves. These hypotheses respectivelyinvolve the temperature excess of the less massive components and spotson the more massive components, and are found to yield similar results.Existing data on other contact binaries in multiple visual systems arediscussed, and it is noted that the contact binaries seem to follow thesame statistical distributions for occurrence in multiples as found fordetached binaries, but severe selection effects limit detectability inmultiple systems for wide orbits having semiaxes below 100 AU.
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CT Eri: Photoelectric Times of Minimum and Improved Period
Not Available
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A catalogue of parameters for eclipsing binaries
Not Available
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57th Name-List of Variable Stars
Not Available
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Results of the Bamberg Southern Hemisphere Sky Patrol [erratum: 1969MNSSA..28...79S]
Not Available
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Elements for Bamberg Variables
Not Available
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Langfristige Periodenkontrolle fur Bedeckungsveranderliche der Bamberger Liste.
Not Available
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Bright Southern BV-Stars
Not Available
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INHABITED SKY
