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J/A+A/437/375   Approximate elements of eclipsing binaries    (Dryomova+, 2005)

Catalog of orbital elements, masses and luminosities of short-periodic RS CVn-type eclipsing systems. Dryomova G.N., Perevozkina E.L., Svechnikov M.A. <Astron. Astrophys. 437, 375 (2005)> =2005A&A...437..375D
ADC_Keywords: Binaries, eclipsing ; Combined data Keywords: binaries: eclipsing - catalogs - stars: fundamental parameters Abstract: The new data on the orbital elements, masses and luminosities have been collected for 31 pre-contact binary systems of short-periodic RS CVn type. The results of statistical treatment of the catalogue data pursue the goal of an accurate definition of the properties and evolutionary status of the given class systems. The ages of pre-contact systems have been estimated by isochrone method. Numerous comments and bibliographic references to the catalogue are accessible. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 169 33 Orbital elements, masses and luminosities of systems of type RS CVn refs.dat 222 112 References
See also: J/A+AS/102/343 : UBVRI polarization of RS CVn-type binaries (Scaltriti+ 1993) V/42 : Close double stars (Svechnikov+, 1984) V/118 : Catalog of eclipsing binaries parameters (Perevozkina+, 1999) V/119 : Catalog of field contact binary stars (Pribulla+, 2003) V/120 : Catalog of early-type contact binaries (Bondarenko+, 1996) V/121 : Catalog of DMS-type eclipsing binaries (Svechnikov+, 1999) Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Seq Sequential number of the star system 5- 12 A8 --- Name Name of precontact system 13 A1 --- n_Name [*] *: variable period 16- 26 F11.9 d Period Orbital period of system 29- 46 A18 --- Sp Spectra SP1+SP2 of the components (1) 48- 51 F4.2 --- q Mass ratio of components 52 A1 --- u_q Uncertainty in q 53 I1 --- n_q [0-2] Remarks on q (2) 56- 59 F4.2 solRad A Orbital major semiaxis 62- 65 F4.2 Sun M1 Mass of first component 66 A1 --- u_M1 Uncertainty in M1 69- 72 F4.2 Sun M2 Mass of second component 73 A1 --- u_M2 Uncertainty in M2 76- 79 F4.2 Sun R1 Radius of first component 80 A1 --- u_R1 Uncertainty in R1 83- 86 F4.2 Sun R2 Radius of second component 87 A1 --- u_R2 Uncertainty in R2 90- 93 F4.2 mag Mbol1 Absolute bolometric magnitudes of first component (3) 96- 99 F4.2 mag Mbol2 Absolute bolometric magnitudes of second component (3) 102-106 F5.3 --- r1 Relative radius of first component in units of Orbital major semiaxis A 109-113 F5.3 --- r2 Relative radius of second component in units of Orbital major semiaxis A 116-120 F5.3 --- L1 Relative luminosity of massive component in units of L1+L2=1 121 A1 --- n_L1 [V] Effective wave length in L1 124-128 F5.2 --- J1/J2 Surface brightness ratio of more massive component to one of less massive (J1/J2) 129 A1 --- n_J1/J2 [V] Effective wavelength in J1/J2 132-136 F5.2 deg i Orbital inclination 139-141 A3 --- W Weight (4) 142 A1 --- u_W Uncertainty in W 145-148 F4.2 Gyr Age Age of precontact system estimated by isochrone method (5) 151-154 F4.2 Gyr e_Age ? rms uncertainty on Age 157-168 A12 --- r_Name References on the key articles, in refs.dat file
Note (1): In the square brackets SP2 computed from the known spectrum SP1 and the ratio J1/J2. Note (2): Note on mass ratio of components is numbered as follows: 0 = if q is found from double-lined spectra; 1 = if q is found from photometrical light-curve; 2 = if q is found by the relation (M-L) with the using mass function from single-lined spectrum. Note (3): Absolute bolometric magnitudes are calculated by their geometrical parameters, spectral and luminosity classes. We used effective temperature scale of Popper, 1980ARA&A..18..115. Note (4): Weight characterizes the reliability of evaluation of photometric and absolute elements in 10-ball scale (highly unreliable elements have weight 0; elements, evaluated with reliability, approaching to reliability of the evaluation of elements by exact methods over their light curves and radial velocity curves have W=9. For systems with certain meaning of SP1 the elements are defined more certainly and they have weight essentially larger than systems with uncertain component spectrum. Note (5): We used evolution models of Maeder & Meynet, 1988A&AS...76..411M.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Ref Reference number 5- 23 A19 --- BibCode BibCode 25- 59 A35 --- Aut Author's name 63-222 A160 --- Com Comments

(End) Veta Avedisova (INASAN) 10-Jan-2005
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