V/42 Close double stars (Svechnikov+, 1984)
Catalog of Orbital elements, Masses and Luminosities of close double stars Svechnikov M.A., Bessonova L.A. <Bull. Inform. CDS 26, 99 (1984)> =1984BICDS..26...99S SIMBAD/NED Reference
ADC_Keywords: Binaries, orbits ; Description: This catalogue is a new edition of the catalogue of the photometric and absolute elements of close double systems by Svechnikov (ref 142). After the appearance of this catalogue(1969), the numerous new data concerning both photometric and spectroscopic elements of orbits of the eclipsing binaries were published. The precision of determination of the light curves of eclipsing systems is essentially augmented; now, the light curves of eclipsing binaries are obtained mainly by means of multicolour photoelectric observations; for a number of systems,e extra-atmospheric observations from satellites and orbital astronomical observatories are available. More details are available in original.txt. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file original.txt 80 414 Original introduction table1.dat 68 246 Summary of close binaries table2.dat 124 483 Photometric elements table3.dat 92 352 Absolute elements notes.txt 80 8468 Notes to tables 2 and 3 refs.txt 80 1688 References acknow.txt 80 27 Acknowledgements
See also: V/118 : Catalog of eclipsing binaries parameters (Perevozkina+, 1999) V/115 : Semidetached and semidetouched eclipsing binaries (Surkova+, 2004) V/121 : Catalog of DMS-type eclipsing binaries (Svechnikov+, 1999) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
2- 20 A19 --- Name Designation of the Eclipsing Binary 26- 33 A8 --- HD Designation in Henry Draper Catalogue 34- 40 A7 --- Type Eclipsing binary type 47- 55 A9 --- Group of classification (see file "original.txt") 59- 61 I3 --- Seq [1/246] Number of the system used in table2 and table3 65- 68 A4 --- Note e.g. other possible class (see "original.txt")
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/246]+= Number of the system 5- 16 A12 --- Name Designation of the System 18- 29 F12.9 d Period [0.2/40]? Period 30- 31 A2 --- n_Period [*?] '*' indicates a variability of Period 33- 38 A6 --- Type of eclipse (see file "original.txt") 41- 46 F6.4 --- R1 ]0/1[? Mean fractional radius (2) 47- 48 A2 --- n_R1 [*:) ] Notes on R1 (1) 51- 56 F6.4 --- R2 ]0/1[? Mean fractional radius (2) 57- 58 A2 --- n_R2 [*:) ] Notes on R2 (1) 60- 64 F5.3 --- b/a [0/1]? Ratio of minor to major axis 65- 66 A2 --- n_b/a [*:) ] Notes on B/A (1) 68- 72 F5.2 deg i ]0/90]? Orbital inclination angle 73- 74 A2 --- n_i [*:) ] Notes on i (1) 76- 79 F4.2 --- LimbCoef [0/1]? Used limb-darkening coefficient (3) 80- 81 A2 --- n_LimbCoef [*:) ] Notes on LimbCoef (1) 84- 89 F6.4 --- L1 [0/1]? Fractional light (relative to L1+L2) 90- 91 A2 --- n_L1 [*:) ] Notes on L1 (1) 93- 98 F6.4 --- L2 [0/1]? Fractional light (relative to L1+L2) 99-100 A2 --- n_L2 [*:) ] Notes on L2 (1) 101-107 F7.3 --- J1/J2 ]0/]? Ratio of surface brightness (4) 108-109 A2 --- n_J1/J2 [*:) ] Notes on J1/J2 (1) 112-117 A6 0.1nm Passband Wavelength domain 119 A1 --- l_Weight Limit flag (<) on Weight 120 I1 --- Weight [0/9]? on the reliability of photometric elements (See Svechnikov, ref 142) 122-124 A3 --- Com Comments (5)
Note (1): The '*' indicates a note (see file notes) the colon ':' a questionable value; bracket ')' very questionable values (the original left bracket has been removed) Note (2): The mean fractional radius (or the small equatorial semi-axes of ellipsoidal stars which are, within the limits of errors of evaluation of photometric elements, practically equal to the mean radii) relative to the orbital major semi-axis Note (3): if the values of the limb-darkening coefficient of the components are not equal, these are given in the notes (file notes) Note (4): ratio of surface brightness found from the photometric solution; if the geometric elements of the system obtained from several different (but very similar) photometric solutions are averaged, J1/J2 are calculated with the averaged values of the radii of the components. Note (5): Figures '1' and '2' designate the cases, when 2 essentially different variants of the photometric solutions for the same eclipsing system exist, and when we are not able to prefer one of these cases (as a rule, however, only those photometric solutions are given) which seem to be (in opinion of the authors of this catalogue) the most realistic. The data concerning the other photometric solutions (or corresponding bibliographic references) are mentioned in the notes.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/246]+= Number of the system 5- 22 A18 --- Sp Spectral classes 24- 28 F5.3 --- q ]0/1]? Mass ratio M2/M1 (2) 29- 30 A2 --- n_q [*:) ] Note on q (1) 32- 36 F5.2 solMass M1 [0.1/60]? Mass of first component 37 A1 --- q_M1 Uncertainty flag (:) on M1 39- 43 F5.2 solMass M2 [0.1/60]? Mass of second component 44 A1 --- q_M2 Uncertainty flag (:) on M2 46- 50 F5.2 solRad a ? Orbital semi-major axis 52- 56 F5.2 solRad Rad1 ? Radius of first star 57- 58 A2 --- n_Rad1 [*:) ] Note on Rad1 (1) 60- 65 F6.3 solRad Rad2 ? Radius of second component 66 A1 --- q_Rad2 Uncertainty flag (:) on Rad2 68- 73 F6.2 mag Mbol1 ? Absolute Bolometric magnitude of component 1 (3) 74 A1 --- n_Mbol1 [!)] Note on Mbol1 (1) 76- 81 F6.2 mag Mbol2 ? Absolute Bolometric magnitude of component 2 (3) 82- 83 A2 --- n_Mbol2 [!:*) ] Note on Mbol2 (1) 85 A1 --- l_W2 Lower limit (<) on W2 86 I1 --- W2 ? Weight on the accuracy of determination of the absolute elements. (4) 87- 92 A6 --- Comment Comments (5)
Note (1): The '*' indicates a note (see file notes) the colon ':' a questionable value; the bracket ')' very questionable values (the original left bracket has been removed) exclamation '!' is not explained in the "original.txt" file Note (2): Mass-ratios found spectroscopically, from double-lined spectroscopic orbit, are not accompanied by additional marks. The values of q estimated by means of the so-called 'M-L method', using the mass-function obtained from single-lined spectral orbit, and assuming,that primary component satisfies the mass-luminosity relation for the main-sequence-stars (see Kopal, ref 371;823; Svechnikov, ref 142), are enclosed in brackets. The values of q estimated by some other method, as well as averaged values oF q, are accompanied by the asterisks. Note (3): The absolute bolometric magnitudes are computed using the geometric and spectroscopic characteristics of the components yielded in the previous columns; the stellar effective temperatures given in Popper's (ref 1615) survey (and based mainly on the scale of effective temperatures and bolometric corrections of Hayes, ref 1623) are used. Note (4): see Svechnikov, ref 142 Note (5): Figures '1' and '2' indicate the cases, when 2 different variants of the absolute elements are obtained (corresponding to 'case 1' and 'case 2' of the evaluation of photometric elements or to 2 considerably different estimates of q). Also,in this column, the number of the group for US-systems is indicated as well as some other important remarks.
Acknowlegement: This document was prepared by Francois Ochsenbein of the CDS in October, 1994. It was modified by the inclusion of the ADC keywords and of a more extensive description.
(End) Nancy G. Roman [ADC] 02-Feb-1995