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J/A+A/455/247    Grid of close binaries experiencing mass exchange (Tian+, 2006)

The blue stragglers formed via mass transfer in old open clusters. Tian B., Deng L., Han Z., Zhang X.B. <Astron. Astrophys. 455, 247 (2006)> =2006A&A...455..247T
ADC_Keywords: Binaries, eclipsing ; Models, evolutionary ; Stars, masses Keywords: Stars: blue stragglers - Stars: binaries: close - Galaxy: open clusters and associations: individual: M67 Description: To simulate the population of the primordial blue stragglers in old open clusters, a grid of close binaries experiencing mass exchange is needed. To this aim, various combinations that can trigger mass exchange for the donor masses of 0.1M to 2.0M are calculated with a fine grid in parameters. The mass range of the accretor is from 0.1M to the mass of the corresponding donor. The mass intervals of the donors and the accretors are all 0.1M. To cover all possible cases of close binaries, the orbit separation ranges from 1.0 to 50.0R with a grid interval of 1.0R. Following the numerical scheme described above, a grid for six ages from 1.0Gyr to 6.0Gyr is obtained. In this table, mass, effective temperature, luminosity, gravity, Hydrogen abundance in the core, Helium abundance in the core, B magnitude, V magnitude, B-V color, mass ratio, orbital separation and period of the close binaries experiencing mass exchange are given. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 277 403 A grid of close binaries experiencing mass exchange
See also: J/A+AS/131/395 : Eclipsing binaries light curves models (Claret 1998) J/AZh/79/259 : Intermediate-Mass Eclipsing Binaries Models (Kovaleva, 2002) J/AZh/79/738 : Binary stars population model in the Galaxy (Tutukov+, 2002) J/ApJ/490/328 : "Mass Discrepancy" for Massive Stars (Burkholder+ 1997) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 F8.4 solMass M1i The initial mass of the accretor 11- 18 F8.4 solMass M2i The initial mass of the donor 24- 29 F6.4 --- qi The initial mass ratio of the binary 32- 37 F6.2 solRad Ai The initial separation of the binary 44- 51 F8.4 d Peri The initial period of the binary 55- 58 F4.1 10+9yr Age The age of the binary 63- 69 F7.4 solMass M1 The mass of the accretor 71- 77 F7.4 [K] logTeff1 The effective temperature of the accretor 81- 88 F8.4 [solLum] logL1 The luminosity of the accretor 93- 99 F7.4 [m/s2] log(g1) The gravity of the accretor 101-106 F6.3 --- H1 The Hydrogen abundance in the core of the accretor 108-113 F6.3 --- He1 The Helium abundance in the core of the accretor 115-122 F8.4 mag Bmag1 B magnitude of the accretor 123-130 F8.4 mag Vmag1 V magnitude of the accretor 131-138 F8.4 --- (B-V)1 B-V color index of the accretor 143-149 F7.4 solMass M2 The mass of the donor 152-157 F6.4 [K] logTeff2 The effective temperature of the donor 161-168 F8.4 [solLum] logL2 The luminosity of the donor 173-179 F7.4 [m/s2] log(g2) The gravity of the donor 181-186 F6.3 --- H2 The Hydrogen abundance in the core of the donor 189-193 F5.3 --- He2 The Helium abundance in the core of the donor 195-202 F8.4 mag Bmag2 B magnitude of the donor 203-210 F8.4 mag Vmag2 V magnitude of the donor 211-218 F8.4 --- (B-V)2 B-V color index of the donor 224-229 F6.4 --- q The mass ratio of the binary 234-239 F6.2 solRad A The separation of the binary 243-250 F8.4 d Per The period of the binary 254-261 F8.4 mag Bmag B magnitude of the binary 262-269 F8.4 mag Vmag V magnitude of the binary 270-277 F8.4 --- B-V B-V color index of the binary
Acknowledgements: Bin Tian, tianbin(at)bao.ac.cn
(End) Bin Tian [NAOC], Patricia Vannier [CDS] 19-Jan-2006
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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