Astrophysics and Space Science

, Volume 181, Issue 2, pp 313–322 | Cite as

Stellar mass-luminosity and mass-radius relations

  • Osman Demircan
  • Göksel Kahraman
Article

Abstract

The new binary star data have been used together with new theoretical estimates in the study of mass-luminosity and mass-radius relations (MLR and MRR) for the Main-Sequence (MS) stars. The slopes of the relations change at certain critical values, e.g., at ∼0.5M⊙ for MLR and at ∼1.7M⊙ for MRR. The first point is the indication of transition from fully-convective internal structure to the developing radiative core, and the second point, the transition from proton-proton cycle to the carbon-nitrogen cycle as the dominant source of nuclear energy in these stars. It seems that these critical points are important in constraining on the stellar models. Improved set of more parameters for stars particularly around the critical points where the slopes of the relations change, may help bringing the theory and observations closer.

Keywords

Internal Structure Theoretical Estimate Nuclear Energy Dominant Source Binary Star 

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Alexander, D. R., Johnson, H. R., and Rypma, R. L.: 1983,Astrophys. J. 272, 773.Google Scholar
  2. Cester, B., Ferluga, S., and Boehm, C.: 1983,Astrophys. Space Sci. 96, 125.Google Scholar
  3. Ciardillo, R. B. and Demarque, P.: 1977,Trans. Astron. Obs. Yale Univ. 33, 1 (CD).Google Scholar
  4. Cox, A. N. and Stewart, J. N.: 1970a,Astrophys. J. Suppl. 19, 243.Google Scholar
  5. Cox, A. N. and Stewart, J. N.: 1970b,Astrophys. J. Suppl. 19, 261.Google Scholar
  6. Eddington, A. S.: 1926,The Internal Constitution of the Stars, Cambridge University Press, Cambridge, reprinted in 1959 by Dover Publ.Google Scholar
  7. Eriksson, K., Gustafsson, B., and Bell, R. A.: 1981, unpublished.Google Scholar
  8. Gimenez, A. and Zamorano, J.: 1985,Astrophys. Space Sci. 114, 259.Google Scholar
  9. Griffiths, S. C., Hicks, R. B., and Milone, E. F.: 1988,J. Roy. Astron. Soc. Can. 82, 1.Google Scholar
  10. Gustafsson, B., Bell, R. A., Erikson, K., and Nordlund, A.: 1975,Astron. Astrophys. 42, 407.Google Scholar
  11. Harmanec, P.: 1988,Bull. Astron. Inst. Czech. 39, 329.Google Scholar
  12. Heintz, W. D.: 1978,Double Stars, D. Reidel Publ. Co., Dordrecht, Holland.Google Scholar
  13. Hertzsprung, E.: 1923,Bull. Astron. Inst. Neth. 2, No. 43.Google Scholar
  14. Kopal, Z.: 1978,Dynamics of Close Binary Systems, D. Reidel Publ. Co., Dordrecht, Holland.Google Scholar
  15. Kurucz, R. L.: 1979,Astrophys. J. Suppl. 40, 1.Google Scholar
  16. Lacy, C. H.: 1979,Astrophys. J. 228, 817.Google Scholar
  17. Maeder, A. and Meynet, G.: 1988,Astron. Astrophys. Suppl. 76, 411.Google Scholar
  18. Magee, N. H., Mertz, A. L., and Heubner, W. F.: 1975,Astrophys. J. 196, 617.Google Scholar
  19. McCluskey, G. E., Jr. and Kondo, Y.: 1972,Astrophys. Space Sci. 17, 134.Google Scholar
  20. Mengel, J. G., Sweigart, A. W., Demarque, P., and Gross, P. G.: 1979,Astrophys. J. Suppl. 40, 733.Google Scholar
  21. Patterson, J.: 1984,Astrophys. J. Suppl. 54, 443.Google Scholar
  22. Popper, D. M.: 1980,Ann. Rev. Astron. Astrophys. 18, 115.Google Scholar
  23. Russell, H. N., Adams, W. S., and Joy, A. H.: 1923,Publ. Astron. Soc. Pacific 35, 189.Google Scholar
  24. Smith, R. C.: 1983,The Observatory 103, 29.Google Scholar
  25. Stagni, R., Margoni, R., and Mammano, A.: 1982,Astrophys. Space Sci. 88, 115.Google Scholar
  26. VandenBerg, D. A.: 1983,Astrophys. J. Suppl. 51, 29.Google Scholar
  27. VandenBerg, D. A. and Bridges, T. J.: 1984,Astrophys. J. 278, 679.Google Scholar

Copyright information

© Kluwer Academic Publishers 1991

Authors and Affiliations

  • Osman Demircan
    • 1
  • Göksel Kahraman
    • 1
  1. 1.Ankara University Observatory, and Department of Astronomy and Space SciencesAnkaraTurkey

Personalised recommendations