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V/120 Catalog of early-type contact binaries (Bondarenko+, 1996)
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Beginning of ReadMe :V/120 Catalog of early-type contact binaries (Bondarenko+, 1996)
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Catalogue of Photometric, Geometric, and Absolute elements of contact binary
stars of the early spectral type.
Bondarenko I.I., Perevozkina E.L.
<Publ. Odessa Obs. 9, 20 (1996)>
=1996IzOde...9...20B
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ADC_Keywords: Binaries, eclipsing ; Combined data
Description:
For the first time the early type contact systems were identified as
an individual class in M.A. Svechnikov's Catalogue [1] in 1969, which
contains 8 systems of this type. The Catalogue of Coch R.H., Plavec M.
and Wood F.B. [2] contains 37 systems of the early spectral type.
According to Svechnikov's classification [3] a primary component (more
massive and hotter) of a CE-system (contact system of early spectral
class) has a spectral class earlier than F0-F2 and an orbital period
of more than 0.5 day. Usually the spectral class of a primary is
earlier than the spectral class of a secondary. Both components fill
their Roche-lobes on 90-100%. The following Catalogue of Svechnikov
M.A. and Bessonova L.A. [4] contains 38 CE-systems. In 1986 Bondarenko
I.I. [5] published the Catalogue of the CE-stars, which contained 83
systems.
Physical characteristics of the CE-stars presented in the list of
catalogues abovementioned, were obtained by different authors by using
different methods of calculation.
We propose the Catalogue of the CE-systems with homogeneous absolute
physical characteristics, that allows to define accurately general
features of this class of binary stars. The comparing of physical
characteristics of the CE-systems with other classes` characteristics
of binary stars can show the possible evolutionary stages of the
CE-systems.
The foundation of absolute elements of the CE-systems are the
photometric observations (on the whole, the latest multicolour
photoelectric, in a few cases photographic and visual observations).
The accuracy of modern photometric observations is high, and generally
they are processed with the help of reliable computer methods both
classical and synthetical methods). But reliable spectral observations
(the ray speed curves) are very scarce, especially for both
components). We have preferred the spectral class of a primary (usually
it is more bright), supposing, that it's spectral class was defined
accurately, and photometric and geometrical elements from light
curves.
All stars from our Catalogue were classified preliminarily as
CE-stars by Svechnikov M.A., Istomin L.F. and Grehova O.A. [6]. We
have supposed both components fill their Roche-lobes and by using the
diagram (q-r[critical]) of Plavec-Kratochvile [7] mass ratio was
obtained.
The absolute elements were obtained by the approximated method of
Svechnikov, which was modernized for CE-stars.
Our Catalogue consist of three parts: photometric, geometrical and
absolute elements of CE-systems. All stars were divided approximately
into two groups: massive (m1>3 solar masses for primary) and
less-massive stars (m1<3 solar masses for primary). A Catalogue has a
Supplement.