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"  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  (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 , 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 . 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:
FileName Lrecl Records Explanations
ReadMe 80 . This file objects.dat 40 3796 Coordinates of objects catalog.dat 146 3796 Data on photometric and absolute elements of eclipsing stars notes.dat 426 806 Notes refs.dat 181 18 References
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
Bytes Format Units Label Explanations
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)
Note (1): GZ Sge and V3476 Sgr have no position.
Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
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)
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.
Byte-by-byte Description of file: notes.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Seq Sequential number 6- 14 A9 --- Name Name 18-426 A409 --- Text Text of the note
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
2- 3 I2 --- Ref Reference number 4 A1 --- --- [.] 6-181 A176 --- Text Text of reference
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) 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 5. The general catalogue of variable stars, See Cat. II/250 6. Svechnikov & Taidakova, 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 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 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 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
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