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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 277 403 A grid of close binaries experiencing mass exchange
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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
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Bytes Format Units Label Explanations
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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
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Acknowledgements: Bin Tian, tianbin(at)bao.ac.cn
(End) Bin Tian [NAOC], Patricia Vannier [CDS] 19-Jan-2006