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The Case for Third Bodies as the Cause of Period Changes in Selected Algol Systems
Many eclipsing binary star systems show long-term variations in theirorbital periods, evident in their O-C (observed minus calculated period)diagrams. With data from the Robotic Optical Transient Search Experiment(ROTSE-I) compiled in the SkyDOT database, New Mexico State University 1m data, and recent American Association of Variable Star Observers(AAVSO) data, we revisit Borkovits and Hegedüs's best-casecandidates for third-body effects in eclipsing binaries: AB And, TV Cas,XX Cep, and AK Her. We also examine the possibility of a third bodyorbiting Y Cam. Our new data support their suggestion that a third bodyis present in all systems except AK Her, as is revealed by thesinusoidal variations of the O-C residuals. Our new data suggest that athird body alone cannot explain the variations seen in the O-C residualsof AK Her. We also provide a table of 143 eclipsing binary systems thathave historical AAVSO O-C data with new values computed from the SkyDOTdatabase.
| Photoelectric Minima of Selected Eclipsing Binaries and Maxima of Pulsating Stars
Not Available
| 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.
| Photoelectric Minima of Some Eclipsing Binary Stars
We present 29 minima observations of 11 eclipsing binaries.
| The Henry Draper Extension Charts: A catalogue of accurate positions, proper motions, magnitudes and spectral types of 86933 stars
The Henry Draper Extension Charts (HDEC), published in the form offinding charts, provide spectral classification for some 87000 starsmostly between 10th and 11th magnitude. This data, being highlyvaluable, as yet was practically unusable for modern computer-basedastronomy. An earlier pilot project (Roeser et al. 1991) demonstrated apossibility to convert this into a star catalogue, using measurements ofcartesian coordinates of stars on the charts and positions of theAstrographic Catalogue (AC) for subsequent identification. We presenthere a final HDEC catalogue comprising accurate positions, propermotions, magnitudes and spectral classes for 86933 stars of the HenryDraper Extension Charts.
| Near-contact binaries
Not Available
| Epochs of minimum light for 27 eclipsing binaries
Sixty-one epochs of minimum light for 27 eclipsing binaries arepresented. Where possible these epochs are compared to existing andreliable light elements. Improved light elements have been computed forWZ And, V417 Aql, ZZ Aur, AP Aur, ACCMi, AX Dra, and XZ Leo. Brief notesare made on the periods of SS Ari, AP Aur, U Cep, and GR Tau. The firstphotoelectric light curves of WZ And and TY Del have been obtained, forwhich solutions will be forthcoming. TZ Dra is identified as being a BDstar, while it is pointed out that FR Vul is probably not a BD star.
| A study of the O'Connell effect in the light curves of eclipsing binaries
In the present consideration of O'Connell's (1951) study of the lightcurve asymmetry between outside eclipse maxima, using UBV photoelectricdata, parametric and nonparametric methods indicate significantcorrelations in at least one color between the size of the asymmetry, onthe one hand, and several additional parameters. These include: thecolor index of the asymmetry, the relative sizes of the hotter andsmaller components, and their distortion, the relative separation of thestars, and the logarithm of the period. The present study data arecharacterized by lower mean amplitudes and a much more even distributionof the asymmetry, with respect to sign, than that of O'Connell, andthere is a tendency for the brighter maximum to be redder, contrary toO'Connell's results. More than one mechanism for the O'Connell effect issuggested.
| 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).
| A catalogue of parameters for eclipsing binaries
Not Available
| Photoelectric photometry of the eclipsing binary BS Vul.
Abstract image available at:http://adsabs.harvard.edu/abs/1979A&AS...35...63D
| Visual minima of eclipsing binaries from Cracow observations in 1920-1950.
Not Available
| Light elements of some eclipsing binaries.
Abstract image available at:http://adsabs.harvard.edu/abs/1962AJ.....67..462K
| Benennung von veränderlichen Sternen
Not Available
| 162 neue Veräderliche
Not Available
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Наблюдательные данные и астрометрия
| Созвездие: | Лисичка |
| Прямое восхождение: | 19h37m26.51s |
| Склонение: | +21°55'50.4" |
| Видимая звёздная величина: | 10.092 |
| Собственное движение RA: | 24.6 |
| Собственное движение Dec: | 43.1 |
| B-T magnitude: | 10.528 |
| V-T magnitude: | 10.128 |
Каталоги и обозначения:
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