J/A+AS/103/67 Evolutionary sequences with MC metallicities (de Loore+ 1994)
Evolutionary sequences for massive close binary stars with Magellanic Cloud
metallicities with Rogers-Iglesias opacities
de Loore C., Vanbeveren D.
<Astron. Astrophys. Suppl. Ser. 103, 67 (1994)>
=1994A&AS..103...67D 1994A&AS..103...67D
ADC_Keywords: Models, evolutionary ; Stars, double and multiple ;
Magellanic Clouds
Keywords: stars: binaries: close - stars: evolution - stars: Wolf-Rayet -
Magellanic clouds
Abstract:
Tables of evolutionary sequences for massive stars with metallicities
Z=0.002 and Z=0.01 in the mass range 9 to 40 M☉ and mass ratios
0.9 and 0.6 are presented. The orbital periods are chosen such that
mass transfer according to case B occurs, i.e. mass exchange after
core hydrogen exhaustion, during semi-detached and contact phases. The
evolutionary code used by de Loore & De Greve (1992A&AS...94..453D 1992A&AS...94..453D)
for galactic massive close binaries was updated, i.e. new
thermodynamic quantities and new opacities were installed. The
evolution of both components is followed simultaneously. Stellar wind
mass loss rates during the OB phase are scaled according to the
radiatively driven wind theory. Wolf-Rayet mass loss rates are assumed
to be independent of metallicity. The models presented here may be
used to interpret and evaluate the observations of Wolf-Rayet stars
and massive binary X-ray sources in the Small and Large Magellanic
Clouds.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
lmc.dat 175 181 LMC abundances (Table3 to Table15)
smc.dat 175 176 SMC abundances (Table16 to Table29)
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Byte-by-byte Description of file: lmc.dat smc.dat
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Bytes Format Units Label Explanations
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1- 2 I2 Sun IM1 Initial mass of the primary
4- 7 F4.1 Sun IM2 Initial mass of the secondary
8- 17 A10 --- Phase See note (1)
19- 30 E12.6 yr Age Evolutionary stage
32- 36 F5.2 solMass M1 Mass of the primary
39- 49 E11.4 solMass/yr ML1 Mass loss rate of the primary
53- 57 F5.3 [K] logTeff1 Effective temperature of the primary
61- 65 F5.3 [solLum] logL1 Luminosity of the primary
67- 71 F5.3 --- XC1 Central hydrogen content of the primary
73- 77 F5.3 --- YC1 Central helium content of the primary
79- 83 F5.3 --- XAT1 Surface hydrogen abundance of the primary
87- 91 F5.2 solRad Rad1 Radius of the primary
94- 98 F5.2 Sun MCC1 Convective core mass of the primary
100-107 F8.4 d Period ? Orbital period
108-113 F6.2 solMass M2 ? Mass of the secondary
115-125 E11.4 solMass/yr ML2 ? Mass loss rate of the secondary
129-133 F5.3 [K] logTeff2 ? Effective temperature of the secondary
137-141 F5.3 [solLum] logL2 ? Luminosity of the secondary
143-147 F5.3 --- XC2 ? Central hydrogen content of the secondary
149-153 F5.3 --- YC2 ? Central helium content of the secondary
155-159 F5.3 --- XAT2 ? Surface hydrogen content of the secondary
163-167 F5.2 solRad Rad2 ? Radius of the secondary
171-175 F5.2 solMass MCC2 ? Convective core mass of the secondary
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Note (1): The different phases is as follows:
ZAMS: Zero Age Main Sequence
RP1: Red Point of the primary component
Xc1=0: end of core hydrogen burning of the primary
RLOFi: onset of a case B of Roche Lobe Overflow
Lmin: minimum luminosity of the primary
Xat<0.76 (SMC, or 0.74 (LMC)): hydrogen abundance of the primary drops
below its initial value
CHeB1i: onset of core helium burning of the primary
VHeB1i: onset of core helium burning of the primary
RLOFf: end of Roche Lobe Overflow
Yc1=0: end of core helium burning of the primary
RP2: red point of the secondary
Xc2=0: end core hydrogen burning of the secondary.
Teffmin2: minimum of the effective temperature of the secondary
Teffmax2: maximum of the effective temperature of the secondary
WNL1,WNE1, WC1 denote the onset of the different Wolf-Rayet phases,
the WNL,WNE and WC-phases of the primary.
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(End) James Marcout [CDS] 09-Sep-1993