Astrophysics and Space Science

, Volume 209, Issue 2, pp 273–283 | Cite as

The interaction between the secondary and the common convective envelope in a contact binary

  • Wang Jianmin 


It has been suggested that a contact system almost certainly cannot exist in static equilibrium undergoing periodic thermal relaxation oscillation. The energy transfer in a common convective envelope (CCE) makes the secondary have a complex structure, so the interaction between the secondary and CCE may play an important role in the structure and evolution of the contact system. The present paper tests the TRO theory and investigates this interaction with polytropic stellar model from the observational datum of 22 contact systems directly. It shows that the A-type systems are expanding with a velocity of 25.04 m yr−1, and the W-type systems are contracting at velocity of 3.10 m yr−1 by the calculations about these contact systems. Also, we calculate the ratio of energy transfer and the interaction coefficient for them. The HS (hot secondary) model is supported by our calculations. These results may help to understand the TRO theory and the W-phenomenon.


Static Equilibrium Energy Transfer Observational Data Interaction Coefficient Thermal Relaxation 
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.


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  1. Binnendijk, L.: 1970,Vistas in Astronomy 12, 217.Google Scholar
  2. Eggleton, al. (eds.): 1976,Structure and Evolution of Close Binary Systems, D. Reidel Publ. Co., Dordrecht, p. 346.Google Scholar
  3. Flannery, B.P.: 1976,Astrophys. J. 205, 217.Google Scholar
  4. Hazlehurst, J.: 1985,Astron. Astrophys. 145, 25.Google Scholar
  5. Hilditch, R. al.: 1988,Monthly Not. Roy. Astr. Soc. 231, 311.Google Scholar
  6. Kähler, H.: 1989,Astron. Astrophys. 209, 67.Google Scholar
  7. Kippenhahn, R. and Weigert, A: 1990,Stellar Structure and Evolution, Springer-Verlag, Berlin, pp. 184–185.Google Scholar
  8. Linnell, A.P.: 1986,Astrophys. J. 300, 304.Google Scholar
  9. Linnell, A.P.: 1987,Astrophys. J. 316, 389.Google Scholar
  10. Lucy, L.B.: 1968,Astrophys. J. 151, 1123.Google Scholar
  11. Lucy, L.B.: 1976,Astrophys. J. 205, 208.Google Scholar
  12. Lucy, L.B. and Wilson, R.E.: 1979,Astrophys. J. 231, 502.Google Scholar
  13. Mochnacki, R.: 1981,Astrophys. J. 245, 650.Google Scholar
  14. Mullan, D.J.: 1975,Astrophys. J. 198, 563.Google Scholar
  15. Robertson, J.A.: 1980,Monthly Not. Roy. Astr. Soc. 192, 263.Google Scholar
  16. Rucinski, S.M.: 1974,Acta Astron. 24, 119.Google Scholar
  17. Sinjab, I.M., Robertson, J.A., and Smith, R.C.: 1990,Monthly Not. Roy. Astr. Soc. 244, 619.Google Scholar
  18. Smith, R.C.: 1983,Observatory 103, 29.Google Scholar
  19. Smith, R.C.: 1984,Quart. J. Roy. Astron. Soc. 25, 405.Google Scholar
  20. Webbink, R.F.: 1977,Astrophys. J. 215, 851.Google Scholar

Copyright information

© Kluwer Academic Publishers 1993

Authors and Affiliations

  • Wang Jianmin 
    • 1
  1. 1.Center for AstrophysicsUniversity of Science and Technology of ChinaHefei, AnhuiChina

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