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V/42 Close double stars (Svechnikov+, 1984)
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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
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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.doc.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
original.doc 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.dat 80 8468 Notes to tables 2 and 3
refs.dat 80 1688 References
acknow.dat 80 27 Acknowledgements
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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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 intro.ori)
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 intro.ori)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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 intro.ori)
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)
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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
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Bytes Format Units Label Explanations
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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)
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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 "intro.ori" 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.
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(End) Nancy G. Roman [ADC] 2-Feb-1995