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J/A+AS/106/275       Theoretical isochrones                     (Bertelli+ 1994)
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Theoretical isochrones from models with new radiative opacities
      Bertelli G., Bressan A., Chiosi C., Fagotto F., Nasi E,
      <Astron. Astrophys. Suppl. Ser. 106, 275 (1994)>
     =1994A&AS..106..275B   (SIMBAD/NED Reference)
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ADC_Keywords: Models, evolutionary; HR diagrams
Keywords: stars: evolution, interiors, fundamental parameters, HR diagram

Abstract:
    In this paper we present large grids of theoretical isochrones for the
    initial chemical compositions [Z=0.0004, Y=0.23], [Z=0.004, Y=0.24],
    [Z=0.008, Y=0.25], [Z=0.02, Y=0.28], and [Z= 0.05, Y=0.352] and ages
    in the range 4Myr to 16Gyr. These isochrones are derived from stellar
    models computed with the most recent radiative opacities by Iglesias
    et al. (1992). In addition to this we present another set with
    chemical composition [Z=0.001, Y=0.23] based on models calculated with
    the radiative opacities by Huebner et al. (1977). All the stellar
    models are followed from the zero age main sequence (ZAMS) to the
    central carbon ignition for massive stars or to the beginning of the
    thermally pulsing regime of the asymptotic giant branch phase (TP-AGB)
    for low and intermediate mass stars. 
    
    For each isochrone, we give the current mass, effective temperatures,
    bolometric and visual magnitudes, (U-B), (B-V), (V-R), (V-I), (V-J),
    (V-H), and (V-K) colors, and the luminosity function for the case of
    the Salpeter law. In addition to this, integrated magnitudes and
    colors at several characteristic points are also presented together
    with the mass of the remnant star when appropriate. The main
    characteristic that makes this set of isochrones very valuable is
    based on their extension in mass and chemical composition, besides the
    calculation of late stages of evolution, beyond the red giant tip till
    the white dwarf stage after the planetary nebula phase.

File Summary:
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 FileName    Lrecl    Records    Explanations
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ReadMe          80          .    This file
table1         106       6369    Model for z=0.0004, Y=0.23
table2         106       5954    Model for z=0.0010, Y=0.23
table3         106       6634    Model for z=0.0040, Y=0.24
table4         106       6709    Model for z=0.0080, Y=0.25
table5         106       6608    Model for z=0.0200, Y=0.28
table6         106       6474    Model for z=0.0500, Y=0.352
z0004.pst       80       8637    Postscript files of table1 ready to print
z001.pst        80       8038    Postscript files of table2 ready to print
z004.pst        80       8844    Postscript files of table3 ready to print
z008.pst        80       8955    Postscript files of table4 ready to print
z02.pst         80       8865    Postscript files of table5 ready to print
z05.pst         80       8625    Postscript files of table6 ready to print
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Byte-by-byte Description of file: table*
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   Bytes Format  Units   Label    Explanations
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   3-  8  F6.3  [yr]  log(Age)    Logarithm of the age
  11- 17  F7.4 solMass   M        Current mass (1) 
  20- 24  F5.3   [K]  log(Teff)   Logarithm of effective temperature
  26- 31  F6.2   mag     Mbol     Bolometric magnitude
  33- 38  F6.2   mag     V        Absolute visual magnitude
  41- 45  F5.2   mag     (U-B)    (U-B) color index
  48- 52  F5.2   mag     (B-V)    (B-V) color index
  55- 59  F5.2   mag     (V-R)    (V-R) color index
  62- 66  F5.2   mag     (V-I)    (V-I) color index
  69- 73  F5.2   mag     (V-J)    (V-J) color index
  76- 80  F5.2   mag     (V-H)    (V-H) color index
  83- 87  F5.2   mag     (V-K)    (V-K) color index
  89- 99  F11.8  ---     FLUM     Luminosity function for the case of the
                                   Salpeter law
 102-106  F5.2  solMass  Mwind    Real value of the mass after mass loss by
                                   stellar wind for massive stars (2)
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Note (1): 
    The current mass is usually increasing along the isochrone, but in the
    transition from the tip of the RGB to the ZAHB and from the tip of the
    AGB to the P-AGB phase. The mass is decreased in these transitions
    according to the effects of mass loss during the RGB phase, and the
    TP-AGB phase as described in section 3.

Note (2):
    For massive stars the actual value of the mass is not given by the
    current mass along the isochrone, but it is derived taking into
    account mass loss by stellar wind as pointed out in section 2.2 
    of the text.
    Of course, for low and intermediate mass stars Mwind is not printed in
    the postscript files, and its value is defined as zero in table* files.
    Only in the youngest isochrones, when massive stars are involved and
    mass loss by stellar wind is taken into account, the value of Mwind
    represents the actual mass associated to the corresponding luminosity
    and effective temperature.
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References:
  Iglesias, C.A., Rogers, F.J., Wilson B.G. =1992ApJ...397..717I
  Huebner, W.F., Merts, A.L., Magee, N.H., Argo, M.F., 1977, 
    Los Alamos Sci. Lab. Rep. LA-6760-M
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(End)                                           Patricia Bauer [CDS] 21-Mar-1994