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J/MNRAS/319/215 Binary evolution (Han+, 2000)
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Low and intermediate-mass close binary evolution and the
initial-final mass relation
Han Z., Tout C.A., Eggleton P.P.
<Mon. Not. R. Astron. Soc. 319, 215 (2000)>
=2000MNRAS.319..215H
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ADC_Keywords: Models, evolutionary ; Binaries, orbits ; Stars, white dwarf
Keywords: binaries: close - stars: evolution - white dwarfs
Description:
Using Eggleton's stellar evolution code, we carry out 150 runs of
Population I binary evolution calculations with the initial primary
mass between 1 and 8 solar masses, the initial mass ratio q=M_1/M_2
between 1.1 and 4, and the onset of Roche lobe overflow (RLOF) at an
early, middle or late Hertzsprung-gap stage. We assume that the RLOF
is conservative in the calculations. We list characteristics for
binaries with different initial parameters at the beginning of RLOF,
minimum luminosity during RLOF, the end of the last episode of RLOF
and the end of the evolutionary calculations. The characteristics
includes the age of the primary, its mass, mass transfer rate, its
effective temperature, its luminosity, its radius, its helium core
mass, its carbon-oxygen core mass, the hydrogen abundance at its
surface, the mass ratio of the binary, and the orbital period.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 92 505 Roche lobe overflow (RLOF) in the Hertzsprung gap
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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2 A1 --- events *[a,b,c,d] events
4- 16 E13.6 yr t1 Primary's age
18- 22 F5.3 solMass M1 Primary's mass
24- 36 E13.6 solMass/yr dM1/dt Mass transfer rate
38- 42 F5.3 [K] log(T1) Primary's effective temperature
44- 49 F6.3 [solLum] log(L1) Primary's luminosity
51- 58 F8.3 solRad R1 Primary's radius
60- 64 F5.3 solMass MHe Primary's helium core mass
66- 70 F5.3 solMass Mco Primary's carbon-oxygen core mass
72- 76 F5.3 --- XH Hydrogen abundance at primary's surface
78- 82 F5.3 --- q Mass ratio of primary to secondary
83- 94 E12.6 d P Orbital period
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Note on events:
The events a, b, c and d are, respectively, the beginning of RLOF,
minimum luminosity during RLOF, the end of the last episode of RLOF and
the end of the evolutionary calculation.
We usually list stellar parameters at a, b, c and d. However, the code
breaks down when RLOF is unstable. In that case, we only list parameters at
a if RLOF is unstable at onset, or at a and b if RLOF is stable at the
onset but becomes unstable after the primary reaches the red giant branch
(RGB)
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Acknowledgements: Zhanwen Han <zhanwen@public.km.yn.cn>
Christopher A. Tout <cat@ast.cam.ac.uk>
Peter P. Eggleton <ppe@ast.cam.ac.uk>
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(End) Zhanwen Han [Yunnan Obs.], Patricia Bauer [CDS] 12-Oct-2000