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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 43 148 Photometric elements table2.dat 126 100 Geometrical and absolute elements notes.dat 80 207 Individual notes
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
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 (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)
Note (2): the systems are the following: UBVRI: Johnson colour system ubvy: instrumental viz: visual pg: photographic
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)
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....36...54R; 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
Byte-by-byte Description of file: notes.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Number of (CE)-system (G1) 5- 80 A76 --- Note Text of the note
Global notes: Note (G1): Numbers from 88 to 100 are assigned to 13 stars from the Supplement
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 7: Plavec & Kratochvil, 1964, Tables for the Roche Model of Close Binaries. 1964BAICz..15..165P.
(End) Arina Teplyakova [Moscow University], Veta Avesnikova [INASAN] 27-Sep-2004
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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