V/120 Catalog of early-type contact binaries (Bondarenko+, 1996)
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 1996IzOde...9...20B
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.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 43 148 Photometric elements
table2.dat 126 100 Geometrical and absolute elements
notes.dat 80 207 Individual notes
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See also:
V/42 : Close double stars (Svechnikov+, 1984)
V/115 : Semidetached and semi-detouched eclipsing binaries (Surkova+, 2004)
V/118 : Catalog of eclipsing binaries parameters (Perevozkina+, 1999)
V/119 : Catalogue of field contact binary stars (Pribulla+, 2003)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Number of (CE)-system (G1)
5- 13 A9 --- Name Designation in General Catalogue of Variable
Stars (4th Edition)
15- 18 F4.2 --- Coef1 ? limb-darkening coefficient
20- 23 F4.2 --- Coef2 ? limb-darkening coefficient
25 A1 --- n_Coef1 [*] *: Approximated values of darkness to
an edge according to the spectral type
27- 31 F5.3 --- L1 ? Fractonal light (relative to L1+L2)
33- 38 F6.3 --- J1/J2 ? Surface brightness ratio of components
40- 43 A4 --- Phot Photometry system of light curve or
effective wavelength which was used for
photoelectric observation (2)
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Note (2): the systems are the following:
UBVRI: Johnson colour system
ubvy: instrumental
viz: visual
pg: photographic
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq Number of (CE)-system (G1)
5- 13 A9 --- Name Designation in General Catalogue of Variable
Stars
15- 21 A7 --- Sp1 The spectral class of primary (2)
23- 29 A7 --- Sp2 The spectral class of secondary (2)
31- 34 F4.1 solMass M1 Mass of primary is determined by the
mass-luminosity relation for stars of the
main sequence
36- 39 F4.1 solMass M2 Mass of secondary is calculated using a
photometric mass ratio q=M1/M2
41- 44 F4.2 --- q Photometric mass ratio derived from the light
curve solution (3)
46- 49 F4.1 solRad R1 Radius of primary
51- 54 F4.1 solRad R2 Radius of secondary
56- 59 F4.1 solRad a Value of the orbital semimajor axis
61- 65 F5.1 mag M1bol Absolute bolometric magnitude of primary
67 I1 --- Wph Weight (10 ball system) (4)
69- 73 F5.1 --- M2bol Absolute bolometric magnitude of secondary
75- 79 F5.3 --- rad1f Fractional radius of the primary from
photometric solutions
81- 85 F5.3 --- rad2f Fractional radius of the secondary from
photometric solutions
87- 90 F4.1 deg i Inclination of the orbital axis to the sight
92- 94 I3 % mu1 Degree of filling of Roche-Lobe of primary
96- 98 I3 % mu2 Degree of filling of Roche-Lobe of secondary
100-103 I4 pc Dist ? Distance to the system
105 I1 --- Wabs Weight (10 ball system) (5)
107-114 F8.5 d Per Sideral orbital period
116 A1 --- n_Per [*] * - variability of period
118-122 A5 --- Type Type of eclipse (6)
124-125 A2 --- Method Method of recognition of photometric
solution (7)
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Note (2): The spectral class of primary was obtained from spectroscopic
observations (in few cases from other relations of physical
characteristics of the system). The spectral class of secondary
appearing in brackets ([B1]) is calculated from photometric ratio
J1/J2, assuming that components radiate as absolutely black bodies.
Note (3): Values deduced on the assumption that the secondary fills
its Roche-lobe.
Note (4): Weight characterizes the quality of photometric element
determination. Details in Svechnikov M.A., 1969.
Note (5): Weight characterizes the degree of reliability of absolute element
system determination (when elements are determined inexact Wabs<1)
Note (6): Type of eclipse:
p. tr. -partial transit
p. oc. -partial occultation.
Note (7): Method of recognition of photometric solution:
* L-Lavrov
* K-Kopal Close Binary Systems.N.Y., 1959, Close Binary Systems
* R-Russel, 1912ApJ....35..315R 1912ApJ....35..315R; 1912ApJ....36...54R 1912ApJ....36...54R;
1912ApJ....36..239R 1912ApJ....36..239R
* RM-Ressel-Merrill, 1952, The determinations of the elements of
eclipsing binaries. - Contribs Princeton Univ. Obs., 26.
* W-Wood, 1953, A finding list for observers of eclipsing variables.
Publ. Univ. Pennsilvania, 8.
* WD-Wilson-Deviney, 1977ApJ...211..853L 1977ApJ...211..853L
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Byte-by-byte Description of file: notes.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Seq Number of (CE)-system (G1)
5- 80 A76 --- Note Text of the note
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Global notes:
Note (G1): Numbers from 88 to 100 are assigned to 13 stars from the Supplement
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References:
1: Svechnikov, 1969, A Catalogue of Orbital Elements, Masses and
Luminosities of Close Double Stars. Sverdlovsk,
Ural State University.
2: Koch, Plavec and Wood, 1970, A Catalogue of Graded Photometric
Studies of Close Binaries.
3: Svechnikov, 1986, The catalogue of orbital elements, masses and
luminosities of close binary stars, Irkutsk, Irkutsk Univ. Publ.
4: Svechnikov & Bessonova, 1984, A Catalogue of Orbital Elements,
Masses and Luminosities of Close Double Stars. CDS Bull 26, 99
(Cat. V/42)
5: Bondarenko, 1986, Astr.- Geodez. Researches, p.49
6: Svechnikov, Istomin and Grehova, 1980PZ.....21..399S 1980PZ.....21..399S
7: Plavec & Kratochvil, 1964, Tables for the Roche Model of Close
Binaries. 1964BAICz..15..165P 1964BAICz..15..165P.
(End) Arina Teplyakova [Moscow University], Veta Avesnikova [INASAN] 27-Sep-2004