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J/A+A/426/1001      Catalog of contact binary stars          (Csizmadia+, 2004)

On the properties of contact binary stars. Csizmadia Sz., Klagyivik P. <Astron. Astrophys. 426, 1001 (2004)> =2004A&A...426.1001C
ADC_Keywords: Stars, double and multiple Keywords: stars: binaries: close - stars: evolution - stars: binaries: eclipsing - catalogs Abstract: A catalogue of light curve solutions of contact binary stars has been compiled. It contains the results of 159 light curve solutions. Properties of contact binary stars were studied by using the catalogue data. As it is well known since Lucy's (1968ApJ...151.1123L, 1968ApJ...153..877L) and Mochnacki's (1981ApJ...245..650M) works, primary components transfer their own energy to the secondary star via the common envelope around the two stars. This transfer was parameterized by a transfer parameter (ratio of the observed and intrinsic luminosities of the primary star). We proved that this transfer parameter is a simple function of the mass and luminosity ratio. This newly found relation is valid for all systems except H type systems which have a different relation. We introduced a new type of contact binary stars: H subtype systems which have a large mass ratio (q>0.72). These systems show highly different behaviour on the luminosity ratio - transfer parameter diagram from other systems and according to our results the energy transfer rate is less efficient in them than in other type of contact binary stars. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2a.dat 298 159 Catalogue of the light curve solutions of W UMA stars table2b.dat 156 198 References table2c.dat 164 50 List of stellar spots on the surfaces of contact binary components table2d.dat 54 13 *Notes on individual systems table3.dat 184 3 Results of light curve solutions made by the BINSYN code
Note on table2d.dat: If different reflection coefficient, limb darkening coefficient or gravity darkening exponent was assumed or measured for the two components, we list them in this table
See also: II/250 : Combined General Catalogue of Variable Stars (Samus+ 2004) V/119 : Field contact binary stars catalog (Pribulla+, 2003) J/AcA/51/259 : Contact binaries in OGLE-I database (Szymanski+, 2001) J/PASP/108/332 : Photometric analysis of contact binaries (Lapasset+ 1996) J/A+A/311/523 : Photometry of W UMa (Maceroni+, 1996) J/A+A/327/1017 : GO Cygni system (Rovithis-Livaniou+ 1997) J/A+A/355/171 : TZ Boo + Y Sex orbital periods (Qian+, 2000) J/A+A/395/587 : GR Tau BV light curves (Zhang+, 2002) J/A+A/403/637 : V and R light curves of GSC 3822-1056 (Csizmadia+, 2003) J/A+A/417/745 : V861 Her V(RI)C differential photometry (Csizmadia+ 2004) J/A+AS/106/373 : AB And UBV photometry (Demicran+, 1994) J/A+AS/122/515 : HL Aur light curves and minima (Zhang+ 1997) J/A+AS/136/139 : VB light curves of YY Eri (Yang+, 1999) J/AJ/109/359 : H235 in NGC 752 (Milone+ 1995) J/AJ/110/2400 : BVI photometry of V728 Her (Nelson+ 1995) J/AJ/116/2549 : HW Per UBV differential photometry (Samec+, 1998) J/PASP/108/338 : UBV obs. of the contact binary BF Pav (Gonzalez+ 1996) Byte-by-byte Description of file: table2a.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Name Name of the contact binary system (1) 15 A1 --- Type [ABHW] Type of the contact binary (2) 20- 21 I2 h RAh Right ascension (J2000.0) (from FK5 or GCVS) 23- 24 I2 min RAm Right ascension (J2000.0) (from FK5 or GCVS) 26- 30 F5.2 s RAs Right ascension (J2000.0) (from FK5 or GCVS) 32 A1 --- DE- Declination sign (J2000.0) (from FK5 or GCVS) 33- 34 I2 deg DEd Declination (J2000.0) (from FK5 or GCVS) 36- 37 I2 arcmin DEm Declination (J2000.0) (from FK5 or GCVS) 39- 43 F5.2 arcsec DEs ? Declination (J2000.0) (from FK5 or GCVS) 45- 57 F13.5 d EphEp Ephemeris epoch. If no recent reliable ephemeris was available, we repeated the one given in GCVS 59- 69 F11.9 d Per The orbital period of the system. If no recent reliable ephemeris was available, we repeated the one given in GCVS. 71- 76 F6.4 --- M2/M1 ?=9.999 The spectroscopically determined mass ratio of the system (3) 77 A1 ---- n_M2/M1 [*] Note on M2/M1 (3) 79- 85 F7.5 --- M2/M1p Photometrically determined mass ratio of the system (4) 86- 92 F7.4 --- FOF ?=9.999 Fill-out factor (5) 93 A1 --- n_FOF [*] Calculated FOF (6) 95-100 F6.3 deg Incl Inclination of the orbital plane of the system using the conventional rule (90 degrees means the edge-on orbit). 102-106 I5 K Ts1 Surface temperature of the primary component. See note (7) 108-112 I5 K Ts2 Surface temperature of the secondary component. See note (7) 115-121 F7.5 --- R1/RT ?=9.999 Average fractional radius of primary component (8) 122 A1 --- n_R1/RT [*] Note on R1/RT (9) 123-129 F7.5 --- R2/RT ?=9.999 Average fractional radius of secondary star (8) 130 A1 --- n_R2/RT [*] Note on R2/RT (9) 131-137 F7.5 --- LU1/LUT ?=9.999 Fractional luminosity of the primary component (L1/Ltot) in Johnson U band (10) 138 A1 --- n_LU1/LUT [ur] If Stroemgren u or r luminosity in LU1/LUT 139-145 F7.5 --- LB1/LBT ?=9.999 Fractional luminosity of the primary component (L1/Ltot) in Johnson B band (10) 146 A1 --- n_LV1/LVT [bv] If Stroemgren b or v luminosity in LV1/LUT 147-153 F7.5 --- LV1/LVT ?=9.999 Fractional luminosity of the primary component (L1/Ltot) in Johnson V band (10) 154 A1 --- n_LR1/LRT [rb] If Stroemgren r or b luminosity in LR1/LUT 155-160 F6.4 --- LR1/LRT ?=9.999 Fractional luminosity of the primary component (L1/Ltot) in Cousins R band (10) 162 A1 --- n_LI1/LIT [y] If Stroemgren y luminosity in LI1/LUT 163-168 F6.4 --- LI1/LIT ?=9.999 Fractional luminosity of the primary component (L1/Ltot) in Cousins I band (10) 171-176 F6.4 --- LU3/LUT ?=9.999 Fractional luminosity of the tertiary component (L3/Ltot) in Johnson U band (11) 178 A1 --- n_LB3/LBT [u] If Stroemgren u luminosity in LB3/LBT 179-184 F6.4 --- LB3/LBT ?=9.999 Fractional luminosity of the tertiary component (L3/Ltot) in Johnson B band (11) 186 A1 --- n_LV3/LVT [v] If Stroemgren v luminosity in LV3/LVT 187-192 F6.4 --- LV3/LVT ?=9.999 Fractional luminosity of the tertiary component (L3/Ltot) in Johnson V band (11) 194 A1 --- n_LR3/LRT [b] If Stroemgren b luminosity in LR3/LRT 195-200 F6.4 --- LR3/LRT ?=9.999 Fractional luminosity of the tertiary component (L3/Ltot) in Cousins R band (11) 202 A1 --- n_LI3/LIT [y] If Stroemgren y luminosity in LI3/LIT 203-208 F6.4 --- LI3/LIT ?=9.999 Fractional luminosity of the tertiary component (L3/Ltot) in Cousins I band (11) 211-215 F5.3 --- Dark ?=9.999 Value of the gravity darkening exponent used in the light curve solution (12) 218 A1 --- l_Reflect Limit flag on Reflect 219-223 F5.3 --- Reflect ?=9.999 Value of the reflection coefficient used in the light curve solution (13) 227-231 F5.3 --- LDCU ?=9.999 Value of the limb darkening coefficient in U used in the light curve solution (14) 233 A1 --- n_LDCU [ur] If Stroemgren u or r band in LDCU 234-238 F5.3 --- LDCB ?=9.999 Value of the limb darkening coefficient in B used in the light curve solution (14) 240 A1 --- n_LDCB [bv] If Stroemgren b or v band in LDCB 241-245 F5.3 --- LDCV ?=9.999 Value of the limb darkening coefficient in V used in the light curve solution (14) 247 A1 --- n_LDCV [rb] If Stroemgren r or b band in LDCV 248-252 F5.3 --- LDCR ?=9.999 Value of the limb darkening coefficient in Rc used in the light curve solution (14) 254 A1 --- n_LDCI [y] If Stroemgren y band in LDCI 255-259 F5.3 --- LDCI ?=9.999 Value of the limb darkening coefficient in Ic used in the light curve solution (14) 261-267 F7.4 --- SP Dimensionless surface potentials of the two components (15) 269-274 F6.3 solRad amaj ?=9.999 Semi-major axis of the system in solar radius 279-298 A20 --- Ref Reference numbers where the above data were taken from, see Tables 1b and 1c as well.
Note (1): The GCVS name is listed. If the star has no final designations in the GCVS, we give a SIMBAD compatible name of the star. Note (2): Four types of contact binaries are used in the catalogue: * A: the larger star is the hotter one. * B: there is more than 1000K temperature difference between the components and q<0.72 (q means the mass ratio). * H: the mass ratio of the system is higher than 0.72 (M2/M1). * W: The smaller star is the hotter one. Note (3): If spectroscopic mass ratio was greater than unity, we list the reciprocal value. An asterisk means that the spectroscopically determined mass ratio was used in the light curve solution (therefore the two mass ratios are identical). If you find two different mass ratios without an asterisk, the spectroscopical mass ratio was generally measured later in time than the light curve solution was made. But in some cases the photometric mass ratio was fitted independently on the previously known spectroscopic mass ratio. In these cases you should check the references! Note (4): If photometric mass ratio was greater than unity, we list the reciprocal value. Note (5): Fill-out factor is defined by: FOF = (OMEGA-OMEGAout)/(OMEGAin-OMEGA_out). Note (6): An asterisk means that the fill-out factor was not given in the original paper but it was calculated by us from the mass ratio and the surface potential given in the original source. Note (7): It can be fixed or adjusted. To see whether fixed or adjusted this quantity check the references! Note (8): Average fractional radius of the primary component, calculated as the average of pole, back and side radii. Note that this radius is not equivalent with the mean radius of the star which can be computed as the radius of the sphere which has the same volume as the star. However, the mean radius is nearly equal to the average fractional radius. Fractional radius is the ratio of the radius of the component and the semi-major axis of the system. Note (9): An * means that the primary and secondary stars were interchanged. Its reason was that in the original paper the mass ratio was found to be larger than unity and we used the convention that the mass ratio should be smaller than 1 and hence we changed the corresponding values. Note (10): If two components were observed in the system, Ltot = L1 + L2, but in case of three components, Ltot = L1 + L2 + L3! Note (11): If it is 9.999 third light was not searched for or there was no observation in this band. If third light is 0., there was a search for third light in the system but it is undetected. See note (10). Note (12): If gravity darkening exponents were determined from the light curve, or different gravity exponents were applied for the two components, we listed these cases in table1e.dat. So you should check table1e.dat. Note (13): If reflection coefficients were determined from the light curve, or different reflection coefficients were applied for the two components, we listed these cases in table1e.dat. So you should check table1e.dat. Note (14): If it was determined from the light curve, or different limb darkening coefficients were applied for to two components, we listed this cases in table1e.dat. So you should check table1e.dat. Note (15): The potentials were assumed to be equal for the two components. The exception are listed in table1e.dat.
Byte-by-byte Description of file: table2b.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Ref Reference number 5- 23 A19 --- BibCode BibCode 25- 55 A31 --- Aut Author's name 57-156 A100 --- Com Comments
Byte-by-byte Description of file: table2c.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Name Name of the system 16- 22 F7.3 deg COLAT1 Colatitude (90 - LAT) of object 1 23 A1 --- --- [,] 24- 30 F7.3 deg COLAT2 ? Colatitude (90 - LAT) of object 2 31 A1 --- --- [,] 32- 33 I2 deg COLAT3 ? Colatitude (90 - LAT) of object 3 36- 42 F7.3 deg LON1 Longitude of object 1 43 A1 --- --- [,] 44- 49 F6.2 deg LON2 ? Longitude of object 2 50 A1 --- --- [,] 51- 53 I3 deg LON3 ? Longitude of object 3 55- 60 F6.3 deg Rad1 Radius of object 1 61 A1 --- --- [,] 62- 66 F5.2 deg Rad2 ? Radius of object 2 67 A1 --- --- [,] 68- 69 I2 deg Rad3 ? Radius of object 3 71- 76 F6.4 --- Tspot/Tphot1 Temperature factor of object 1 77 A1 --- --- [,] 78- 82 F5.3 --- Tspot/Tphot2 ? Temperature factor of object 2 83 A1 --- --- [,] 84- 87 F4.2 --- Tspot/Tphot3 ? Temperature factor of object 3 89 I1 --- Loc1 [1/2] First location of the spot (1) 90 A1 --- --- [,] 91 I1 --- Loc2 [1/2]? Second location of the spot (1) 92 A1 --- --- [,] 93 I1 --- Loc3 [1/2]? Third location of the spot (1) 95-113 A19 --- BibCode Reference bibcode for the spot 115-138 A24 --- Aut Author's name of the reference 140-164 A25 --- Comment Comments on the reference
Note (1): Number of the star on which the spot is,
Byte-by-byte Description of file: table2d.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Name 10- 13 F4.2 --- g2 ?=9.99 Gravity darkening exponent of the secondary component 15- 19 F5.3 --- A2 ?=9.999 Albedo of the secondary component 21- 25 F5.3 --- x2U ?=9.999 Limb-darkening coefficients for the secondary in Johnson U band 27- 31 F5.3 --- x2B ?=9.999 Limb-darkening coefficients for the secondary in Johnson B band 33- 37 F5.3 --- x2V ?=9.999 Limb-darkening coefficients for the secondary in Johnson V band 39- 43 F5.3 --- x2R ?=9.99 Limb-darkening coefficients for the secondary in Cousins R band 44- 47 F4.2 --- x2I ?=9.99 Limb-darkening coefficients for the secondary in Cousins I band 49- 54 F6.4 --- Omega2 ?=9.999 Dimensionless surface potential for the secondary
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Name Name of the contact binary system 9 A1 --- Type [W] Type of the contact binary (1) 11- 12 I2 h RAh Right ascension (J2000.0) 14- 15 I2 min RAm Right ascension (J2000.0) 17- 23 F7.4 s RAs Right ascension (J2000.0) 25 A1 --- DE- Declination sign (J2000.0) 26- 27 I2 deg DEd Declination (J2000.0) 29- 30 I2 arcmin DEm Declination (J2000.0) 32- 37 F6.3 arcsec DEs Declination (J2000.0) 39- 50 F12.4 d EphEp Ephemeris epoch 52- 60 F9.7 d Per The orbital period of the system 62- 65 F4.2 --- M2/M1 ?=9.99 Spectroscopic mass ratio 67- 72 F6.4 --- M2/M1p Photometric mass ratio 74- 78 F5.3 --- FOF Fill-out factor 80- 84 F5.2 deg Incl Inclination 86- 89 I4 K Ts1 Surface temperature of the primary component 91- 94 I4 K Ts2 Surface temperature of the secondary 96- 97 I2 --- Albedo ?=99 Albedo which was used during the light curve solution. (Fixed value) 99-102 F4.2 --- Dark ?=9.99 Gravity darkening which was used during the light curve solution (Fixed value) 104-107 F4.2 --- LDC ?=9.99 Limb-darkening coefficient used in the light curve solution (Fixed value) 109-112 F4.2 10+6km amaj ?=9.99 Semi-major axis 114-184 A71 --- Ref References
Note (1): W: The smaller star is the hotter one.
Acknowledgements: Szilard Csizmadia, csizmadi(at)konkoly.hu History: * 07-Oct-2004: Original version * 19-Sep-2005: UW CMa modified into UW UMa in table2a.dat
(End) Patricia Vannier [CDS] 07-Oct-2004
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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