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J/A+AS/103/67     Evolutionary sequences with MC metallicities  (de Loore+ 1994)
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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
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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_{sun}_ 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)
    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