Structural Models for Beta Lyrae-Type Disks

  • R. E. Wilson
Part of the Astrophysics and Space Science Library book series (ASSL, volume 98)


Equilibrium structural models are computed for a thick, self-gravitating disk in a binary system. Accretion onto the star is limited by the star’s rapid rotation (the system is a double-contact binary). The potential formulation is taken from a previous paper, and represents the gravitational potential as that of a massive wire. Corrections to the stellar structure differential equations for the distorted geometry are applied, and the equations are integrated and solved by the fitting point method. The energy is supplied by viscosity. Energy transfer is by convection, and is appreciably superadiabatic throughout the disk. A mass of 0.5 M⊙ is assumed. Representative results are: “central” temperature, 67000 K; “central” pressure, 5 × 1011 dynes/cm2; “equal volume” radius, 17 R⊙; luminosity, 5 × 103 L⊙. The model “radius” is in excellent agreement with the observational value for β Lyrae. The model luminosity is slightly higher than the available rate of expenditure of gravitational energy, indicating that a lower disk mass (perhaps 0.25 M⊙) should be tried.


Central Star Main Sequence Star Stellar Structure Normal Star Toroidal Shell 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. Allen, C. W.: 1973, Astrophysical Quantities, 3rd ed. (London: Athlone Press).Google Scholar
  2. Baker, N. H. and Kippenhahn, R.: 1962, Zt. f. Astrophys. 54, p. 114.ADSzbMATHGoogle Scholar
  3. Baker, N. H. and Temesvary, S.: 1966, “Tables of Convective Stellar Envelope Models” (New York: NASA Goddard Institute of Space Studies) (BT).Google Scholar
  4. Bohm-Vitense, E.: 1958, Zt. f. Astrophys. 46, p. 108.ADSGoogle Scholar
  5. Haselgrove, C. B. and Hoyle, F.: 1956, Mon. Not. R. Astr. Soc. 116, p. 515.MathSciNetADSGoogle Scholar
  6. Huang, S.: 1963, Astrophys. J. 138, p. 342.ADSCrossRefGoogle Scholar
  7. Kippenhahn, R. and Thomas, H-C.: 1970, in “Stellar Rotation”, ed. A. Slettebak (Dordrecht: Reidel), p. 20 (KT).CrossRefGoogle Scholar
  8. Packet, W.: 198l, Astr. and Astrophys. (preprint).Google Scholar
  9. Plavec, M.: 1980, U.C.L.A. Astr. and Astrophys. Preprint No. 86.Google Scholar
  10. Sahade, J., Huang, S., Struve, O., and Zebergs, V.: 1959, Trans. Amer. Phil. Soc., 49, Part 1.Google Scholar
  11. Schwarzschild, M.: 1958, “Structure and Evolution of the Stars” (Princeton: Princeton Univ. Press).Google Scholar
  12. Wilson, R. E.: 1974, Astrophys. J. 189, p. 319.ADSCrossRefGoogle Scholar
  13. Wilson, R. E.: 1979, Astrophys. J. 234, p. 1054.ADSCrossRefGoogle Scholar
  14. Wilson, R. E. and Lapasset, E.: 198l, Astr. and Astrophys. 95, p. 328.ADSGoogle Scholar
  15. Wilson, R. E.: 198l, Astrophys. J. 251, (in press for issue of Dec. l) (Paper 1).Google Scholar

Copyright information

© D. Reidel Publishing Company 1982

Authors and Affiliations

  • R. E. Wilson
    • 1
  1. 1.Department of AstronomyUniversity of FloridaUSA

Personalised recommendations