V/124 Approximate elements of eclipsing binaries (Svechnikov+, 1990)
Catalogue of approximate photometric and absolute elements of eclipsing
variable stars.
Svechnikov M.A., Kuznetsova Eh.F.
<Ural university publication, Sverdlovsk, vols 1,2 (1990)>
ADC_Keywords: Binaries, eclipsing; Combined data
Abstract:
In 1986 Svechnikov M.A. had published the "Catalogue of orbital
elements, masses and luminosities" [1] of 246 eclipsing binary systems
with known photometric and spectroscopic elements on comparatively
early stages of their evolution (on the stage of the main sequence and
during or after the "first change of mass") and belonging to DM, SD,
DS, KE, KW, DW and AR evolutionary types (see lower) according to
Svechnikov's classification [2,3,4]. However the representative
eclipsing systems in this catalogue make up only a small share (about
5%) from discovered ones to all eclipsing variable stars of mentioned
types (the general catalogue of variable stars [5] (which is called
further GCVS IV) contains the information approximately of about 5000
eclipsing binary stars of different types). It is of a great interest
for statistic research to give if only the approximate estimations of
relative and absolute elements of those systems for which elements of
the spectroscopic orbits are unknown and the direct calculation of
their absolute characteristics is impossible. For this approximate
estimation the statistic relations (mass - luminosity, mass - radius,
mass - spectrum etc.) obtained for the components of different type
systems [6-9] and a number of other statistic dependences which have
been found from study of 246 eclipsing systems mentioned (for example,
the dependence of orbital inclination I on the depth of main minimum
A1, the dependence of the main component spectral classes for the KE-
and KW-systems on the period P etc.) were used.
For definition of the approximate elements it was used the information
from GCVS IV about the morphological type of systems (EA, EB, EW), its
period, the spectral classes of systems, amplitudes A1 and A2 of the
main and second minima, duration of eclipse D1 and duration of
constant light phase D2 in the main minimum etc., it was made the
classification of eclipsing variable stars with the help of a simple
test, worked out in [4], and the statistic dependences obtained for
the stars of a given type was used later on the question about
reliability of approximate relative and absolute elements which have
been founded by this way was studied earlier in [8]. The accuracy of
these elements is essentially higher for systems with certain spectra
of main components (SP1). This fact was taken into account in
catalogue by giving the essentially a higher weights to elements of
those systems. There are about 1200 systems with the certain meaning
SP1 in our catalogue, it is about 1/3 from all eclipsing systems in
it. On the whole the elements (with different reability) for about
3800 eclipsing variable stars of DM, SD, DS, KE, KW and DW types are
given in catalogue which makes up the overwhelming majority of
eclipsing variable stars with the certain period from GCVS IV.
Because of the possible mistakes in our classification wrong or
incomplete data given in GCVS IV and also because of the fact that
used statistic dependences for definition of elements have an
approximate character, it should be expect that founded in catalogue
the approximate elements for many systems are inaccurate and even
wrong. By our estimation, elements will be grossly wrong for about
10-15% of systems given in this catalogue (which principally have a
small weights), for about 20- 25% of systems the founded elements will
turn out essentially different from veritable, however, we hope that
for 60-70% of systems the photometric and absolute elements will turn
out quite similar to elements which will be received the more exact
methods later on.
The elements, given in catalogue, may be used in the different
statistic researches and also as an initial approximation for the
calculation of photometric and absolute elements of these eclipsing
stars with more exact methods.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
objects.dat 39 3796 Coordinates of objects
catalog.dat 146 3796 Data on photometric and absolute elements of
eclipsing stars
notes.dat 426 806 Notes
refs.dat 180 18 References
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See also:
II/250 : Combined General Catalogue of Variable Stars (Samus+ 2004)
II/150 : Parameters of eclipsing binaries (Brancewicz+, 1980)
V/46 : Classical (Evolved) Algol-Type Binary Candidates (Budding 1984)
V/115 : Semidetached and semidetouched eclipsing binaries (Surkova+, 2004)
V/118 : Catalog of eclipsing binaries parameters (Perevozkina+, 1999)
V/119 : Catalogue 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: objects.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh ? Right ascension (J2000.0)
4- 5 I2 min RAm ? Right ascension (J2000.0)
7- 10 F4.1 s RAs ? Right ascension (J2000.0)
12 A1 --- DE- Declination sign (J2000.0)
13- 14 I2 deg DEd ? Declination (J2000.0)
16- 17 I2 arcmin DEm ? Declination (J2000.0)
19- 20 I2 arcsec DEs ? Declination (J2000.0)
25- 28 I4 --- Seq Number of star system
31- 39 A9 --- Name Object name (1)
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Note (1): GZ Sge and V3476 Sgr have no position.
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Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Seq Number of star system (1)
5 A1 --- Note [*] Remarks on Seq (2)
7- 15 A9 --- Name Name of eclipsing binary (3)
17- 29 F13.9 d Period Orbital period of system
31 A1 --- n_Period [*:?] Remark on Period (4)
33- 47 A15 --- Sp Spectra SP1+SP2 of the components (5)
49- 51 A3 --- Type Eclipsing system type (6)
52 A1 --- u_Type [:] Uncertainty flag on Type
54- 55 A2 --- EType Evolutionary type (7)
56 A1 --- u_EType [:] Uncertainty flag on EType
58- 62 F5.3 --- q Mass ratio of components
64- 69 F6.2 solRad A Orbital major semiaxis (in solar radii)
71- 75 F5.2 solMass M1 Mass of first component
77- 81 F5.2 solMass M2 Mass of second component
83- 87 F5.2 solRad R1 Radius of first component
89- 93 F5.2 solRad R2 Radius of second component
95-100 F6.2 mag Mbol1 Absolute bolometric magnitude of first
component (8)
102-107 F6.2 mag Mbol2 Absolute bolometric magnitude of second
component (8)
109-113 F5.3 --- r1 Relative radius of first component in units of
Orbital major semiaxis A (9)
115-119 F5.3 --- r2 Relative radius of second component in units
of Orbital major semiaxis A (9)
121 A1 --- l_L1 [>] Limit symbol on L1
122-125 F4.2 --- L1 Relative luminosity of massive component in
units of L1+L2=1
126 A1 --- u_L1 [:] Uncertainty flag on L1
127 A1 --- l_J1/J2 [>] Limit symbol on J1/J2
128-134 F7.2 --- J1/J2 Surface brightness ratio of more massive
component to one of less massive (J1/J2) (10)
135 A1 --- e_J1/J2 [:] Uncertainty in J1/J2
137 A1 --- Band [VPvB] Photometric system in J1/J2
139-140 A2 --- l_Incl [≥ ~] Limit flag on Incl
141-144 F4.1 deg Incl Orbital inclination
146 I1 --- W [0/9] Weight (11)
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Note (1): Numbers beginning from 4001 indicate stars taken from a
supplementary table (Svechnikov, Kuznetsova 1990, vol.2, p.224).
Systems 1043, 1143, 1970, 2860, 3598 are excluded from the electronic
version according to Svechnikov's notes (2004, private communication).
Note (2): Asterisk indicates the presence of this system in the notes.dat file.
Note (3): The systems are placed in the catalogue by constellations as in
GCVS IV.
Note (4): The symbol means the following:
: = period is uncertain
* = variable period
? = probably variable period
Note (5): SP1 is given from GCVS IV or from another (as usually, later)
literature. In the last case the spectra from GCVS IV is given in
remarks. The spectral types of components computed from the
observational values of J1/J2 in assumption that both components
radiate as the black bodies are given in the square brackets.
If SP1 is not known from the available literature and it is evaluated
from the statistical dependences for the eclipsing binaries of
different types we put it in brackets ().
If there is in literature only spectral class (for example A or F)
without spectral subclass, then we put in brackets () supposed
spectral subclass (for example A(3)).
Note (6): Eclipsing system type taken from GCVS IV or from other
literatures (E, EA, EB, EW or ELL (rotating))
Note (7): Evolutionary type according to Svechnikov's classification [2,3,4]:
DM = detached main sequence systems. Both components are main sequence
stars, which do not fill their inner Roche lobes.
SD = semi-detached systems, where more massive component is main
sequence star, and less massive secondary component is subgiant
which fills (or nearly fills) its Roche lobe.
DS = detached systems with subgiant secondary. The less massive
subgiant component distinctly does not fill its Roche lobe.
KE = contact systems of early spectra, both components are close to
their Roche lobes, spectra of the more massive component are
not later about F0.
KW = contact systems of W UMa-type with the periods shorter than
0.5 days and with SP1 later than about F0.
DW = systems, similar to W UMa-stars, where both components do not
fill their Roche lobes and their physical characteristics
are similar to those of KW-systems [2,8].
Lately designation of these eclipsing binaries as
"short-periodic RS CVN-type systems" is widely applied [10,11].
Note (8): The effective temperature scale given in [12,13]
Note (9): Radii or the small equatorial semiaxes for ellipsoidal star
(in units of Orbital major semiaxis A).
The index "1" always is related to more massive star.
Note (10): As a rule, in the color of amplitudes of minima A1 and A2
given in GCVS IV)
Note (11): 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.
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Byte-by-byte Description of file: notes.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Seq Sequential number
6- 14 A9 --- Name Name
18-426 A409 --- Text Text of the note
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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2- 3 I2 --- Ref Reference number
4 A1 --- --- [.]
6-180 A175 --- Text Text of reference
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History:
* 26-Jan-2004: Original version
* 04-Feb-2010: (communicated by S. Derriere)
EL Car appeared twice, the 2nd occurence was changed into FL Car and
its position was corrected in file "objects.dat" (from Simbad)
* 20-Nov-2010: Coordinates for MU Gem (#1836) corrected thanks
to Eric Mamajek comment.
References:
1. Svechnikov, A catalogue of orbital elements, masses and luminosities of
close binary systems. Irkutsk: Irkutsk University publ., 1986 p.225.
2. Svechnikov, A catalogue of orbital elements, masses and luminosities
of close binary systems. Uchenie Zapiski UrGU (Sverdlovsk), 1969, n88,
seriya Astronomiya, Issue 5, p.179.
3. Svechnikov & Snezhko, The characteristics and evolution of close binary
systems. Unsteady phenomens and star evolution, M.: Nauka, 1974, p.181.
4. Svechnikov, Istomin & Grekhova, 1980PZ.....21..399S 1980PZ.....21..399S
5. The general catalogue of variable stars, See Cat. II/250
6. Svechnikov & Taidakova, 1984AZh....61..143S 1984AZh....61..143S
7. Svechnikov, Bull. of Abastumanskaya astrophys. obs., 1985. n59. p.71.
8. Svechnikov, dis. ...doct.phys.-mat.science. m., 1985. part.2, 3,
appendix.
9. Svechnikov M.A. Star clusters. Sverdlovsk, 1987. p.158.
10. Hall, 1972PASP...84..323H 1972PASP...84..323H
11. Hall D.S. Multiple periodic variable stars. IAU colloq. n29. Budapest,
1975; ed. Dordecht; Boston, 1976. pt.1. p.287.
12. Popper, 1980ARA&A..18..115P 1980ARA&A..18..115P
13. Hayes D.S., The HR-diagram. IAU symp. n80;ed. Philip A.G.D. and Hayes
D.S. Dordrecht, Reidel, 1978. p.65.
14. Cester et al., 1979MmSAI..50..551C 1979MmSAI..50..551C
15. Gaposchkin S., Veroff. Sternw. Berlin ; Babelsberg, 1932. v.9, n5.
16. Gaposchkin S., Payne-Gaposchkin C. Variable stars, Harvard obs. monographs.
1938. n5.
17. Kopal Z., Shapley M.B., Ann. Jordell Bank obs. 1956. v.1, n4. p.141.
18. Shapley H., Contrib. Princeton Univ. obs. 1915. n3.
(End) Oleg Malkov, Valentin Reva, Veta Avedisova (INASAN) 26-Jan-2004