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J/A+A/285/473     Low-mass stars                               (Forestini 1994)
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Low-mass stars: pre-main sequence evolution and nucleosynthesis; Abundances
     Forestini M.
    <Astron. Astrophys. 285, 473 (1994)>
    =1994A&A...285..473F
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ADC_Keywords: Stars, pre-main sequence; Mass loss; Models, evolutionary; 
Keywords: stars: pre-main sequence - stars: evolution of - nucleosynthesis -
          stars: abundances

Abstract:
   New evolutionary sequences for low-mass (0.5M_{sun}_ <=M_*_ <= 2.5M_{sun}_) 
   pre-main sequence stars of two different metallicities (Z = 0.02 and 0.04) 
   are presented, making use of the most recent physical ingredients. 
   Nucleosynthesis is also followed in detail. Furthermore, we determine the 
   theoretical uncertainties engendered by various treatments of the surface 
   conditions that significantly affect predictions concerning the evolution 
   and the light element surface depletion of these stars. The detailed 
   comparison with observations mainly indicate that (i) it is quite hazardous
   to determine masses of T Tauri stars with a precision of less than about 
   0.3M_{sun}_ given the theoretical uncertainties, (ii) the same conclusion 
   holds, to a less extent, for age determinations, especially if the 
   metallicity of the observed stars is not accurately measured and (iii) while
   we find a very good agreement with the observed Li - T_eff_correlation for 
   the Hyades open cluster, we overestimate the level of Li depletion for the 
   Pleiades. Suggestions are made about this problem. More particulary, at the
   end of the pre-main sequence phase, our solar model (that we fit with 
   {alpha}= 1.5 and Z/X = 0.02744) still keeps in the convective envelope 34% 
   of its initial ^7^Li content. This is quite lower than some of the other 
   works with which we have compared. 

File Summary:
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 FileName    Lrecl    Records    Explanations
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ReadMe          80          .    This file
table1          78        554    Evolutionary sequences
table1.tex      80       1176    LaTex version of table1
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Byte-by-byte Description of file: table1
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   Bytes Format  Units   Label    Explanations
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   1-  3  F3.1   solMass M        Total mass
   5- 10  F6.4   Sun     Z        Star metallicity
      11  A1     ---     n        Note (1)
  14- 18  F5.3  [yr]     log(t)   Star age
  20- 24  F5.2   solLum  L*       Total luminosity
  26- 30  F5.2   solRad  R        Total radius
  32- 36  I5     K       Teff     Effective temperature
  38- 42  F5.1   %       Lnuc     Energetic contribution of the nuclear reaction
                                     in units of L*
  44- 48  F5.1   %       Lgrav    Gravitational energy release (>0)
                                     or absorption (<0) in units of L*
  50- 54  F5.3   solMass Mcore    Mass of the radiative core
  56- 60  F5.3   [K]     logTb    Temperature at the base of the convective
                                   envelope
  62- 66  F5.3   ---     6Li      Surface 6Li abundance
                                     (relative to its initial value)
  68- 72  F5.3   ---     7Li      Surface 7Li abundance
                                     (relative to its initial value)
  74- 78  F5.3   ---     9Be      Surface 9Be abundance
                                     (relative to its initial value)
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Note (1):
      a: with low-temperature radiative opacity tables of Alexander (1983)
      b: with low- and high-temperature radiative opacity tables of
         Alexander (1983) and Huebner et al. (1977), respectively
      c: with the atmospheric temperature stratification given by the analytic
         T(tau) relation of Henyey et al. (1985)
      d: with the atmosphere integrated up to an optical depth tau = 0.001
      e: with alpha = 2
      f: with alpha = 1
      g: with mass accretion from the beginning and during 2.5 10+6 yr, at a
         rate of 10-7 Msun/yr
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(End)                                           Patricia Bauer [CDS] 27-Jan-1994