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J/A+AS/123/273      Illumination in binaries                     (Hameury+, 1997)
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Illumination in binaries
      Hameury J.M., Ritter H.
      <Astron. Astrophys. Suppl. Ser. 123, 273 (1997)>
      =1997A&AS..123..273H      (SIMBAD/NED BibCode)
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ADC_Keywords: Accretion
Keywords: accretion, accretion discs - stars: binaries: close - X-rays: stars -
          methods: numerical

Description:
    We give a simple, but accurate method that can be used to account for
    illumination in compact binary systems which have a low-mass
    companion, even if spherically symmetric illumination of the secondary
    star (not necessarily on the main sequence) is not assumed. This is
    done by introducing a multiplicative factor {PHI} in the
    Stefan-Boltzmann surface boundary condition, which accounts for the
    blocking of the intrinsic secondary flux by X-ray heating of the
    photospheric layers. Numerical fits and tables for {PHI} are given for
    unperturbed effective temperatures in the range 2500-5600K and logg in
    the range 1.0-5.0.

File Summary:
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  FileName      Lrecl  Records   Explanations
--------------------------------------------------------------------------------
ReadMe             80        .   This file
table1             22   232875   Function G(x)
table2             52    10304   Coefficients of the fit of the modified
                                  Stefan-Boltzmann surface boundary condition.
--------------------------------------------------------------------------------

Byte-by-byte Description of file: table1
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  Bytes Format Units  Label      Explanations
--------------------------------------------------------------------------------
  1-  4  F4.2 [cm/s2] logg       Surface gravity
  6-  9  F4.2 [K]     log(Teff)  Effective temperature of the unilluminated star
 11- 14  F4.2  ---    log(1+x)   log(1+x) where x is the illuminating flux in
                                 units of the unperturbed stellar flux
 16- 22  F7.5  ---   log(1/G(x)) -log(G(x)) where G is the fraction of the
                                 interior flux that is not blocked by
                                 illumination
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Byte-by-byte Description of file: table2
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   Bytes Format Units  Label     Explanations
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   1-  3 F3.1   ---    R2/a      Ratio of the secondary radius versus
                                  orbital separation (f2=R2/a)
   5-  8 F4.2  [cm/s2] logg      Surface gravity
  10- 13 F4.2  [K]     log(Teff) Effective temperature of the unilluminated star
  15- 26 E12.5  ---     a1       Coefficient a1 of the polynomial fit of the
                                  modified boundary condition
  28- 39 E12.5  ---     a2       Coefficient a2 of the polynomial fit of the
                                  modified boundary condition
  41- 52 E12.5  ---     a3       Coefficient a3 of the polynomial fit of the
                                  modified boundary condition
--------------------------------------------------------------------------------

Acknowledgements: Jean Marie Hameury <hameury@astro.u-strasbg.fr>
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(End)                                         Patricia Bauer [CDS]   24-Sep-1996