Hostname: page-component-7479d7b7d-8zxtt Total loading time: 0 Render date: 2024-07-09T07:27:16.676Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of Stars in the Post-Main Sequence Stage

Published online by Cambridge University Press:  12 April 2016

R. Kippenhahn
R. Kippenhahn*
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, Institut für Astrophysik, 8046 Garching b. München

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

I would like to start with a short historical introduction. In 1938 thermonuclear reaction rates for hydrogen burning became available. This made it possible to fit a convective core into the point source model of stellar structure integrated by Cowling three years earlier. The free parameter in the fitting process could be fixed with the thermonuclear reaction rates, the first realistic stellar model for a massive main sequence star was constructed! After the war electronic computers became available, and one was able to do more complicated models like those on the lower main sequence, like realistic models for the sun with its helium enriched interior, and one tried already to follow in time the exhaustion of hydrogen in the central regions of stars numerically. There was not too much progress for stars at the upper end of the main sequence. As soon as the stellar model tried to leave the main sequence and to march towards the region of the red supergiants the methods known at that time failed to produce models. For less massive stars the exhaustion of hydrogen could be followed up more easily and, in 1955, the great paper by Hoyle and Schwarzschild came out, which showed how these stars from the main sequence move into the red giant branch and move up parallel to what we now call the Hayashi line (which was not yet known at that time). But when helium started to burn the methods also failed.

Type
Part I: Evolution of Stars in the Post-Main Sequence Stage
Information
International Astronomical Union Colloquium , Volume 69: Binary and Multiple Stars as Tracers of Stellar Evolution , 1982 , pp. 3 - 18
Copyright
Copyright © Reidel 1982

References

van Albada, T.S., Baker, N., 1972, The Evolution of Pop. II Stars, Davis, Philip A.G. (ed.), p. 193.Google Scholar
Becker, S.A., Iben, I., 1980, Astrophys. J. 237, 111.CrossRefGoogle Scholar
Boesgaard, A., 1977, Pubi. Astron. Soc. Pacific 88, 353.CrossRefGoogle Scholar
Cole, P.W., Deupree, R.G., 1980, Astrophys. J. 239, 284.Google Scholar
Cole, P.W., Deupree, R.G., 1981, Astrophys. J. 247, 607.Google Scholar
Demarque, P., Mengel, J.G., 1971, Astrophys. J. 164, 317.CrossRefGoogle Scholar
Fujimoto, M.Y., Nomoto, K., Sugimoto, D., 1976, Pubi. Astr. Soc. Japan 28, 89.Google Scholar
Gingold, R.A., 1974, Astrophys. J. 193, 177.Google Scholar
Hofmeister, E., 1967, Z. f. Astrophys. 65, 194.Google Scholar
Hofmeister, E., Kippenhahn, R., Weigert, A., 1964a, Z.f.Astrophys. 59, 215.Google Scholar
Hofmeister, E., Kippenhahn, R., Weigert, A., 1964b, Z.f.Astrophys. 59, 242.Google Scholar
Hofmeister, E., Kippenhahn, R., Weigert, A., 1964c, Z.f.Astrophys. 60, 57.Google Scholar
Hoyle, F., Schwarzschild, M., 1955, Astrophys. J. Suppl. 2, 1.CrossRefGoogle Scholar
Iben, I., 1964, Astrophys. J. 140, 1631.Google Scholar
Iben, I. Jr., 1967a, Ann. Rev. Astr. Astrophys. 5, 571.Google Scholar
Iben, I., 1974, Ann. Rev. Astr. Astrophys. 12, 215.Google Scholar
Iben, I., 1975a, Astrophys. J. 196, 525.Google Scholar
Iben, I., 1975b, Astrophys. J. 196, 549.Google Scholar
Iben, I., 1976, Astrophys. J. 208, 165.Google Scholar
Iben, I., 1972, The Evolution of Pop. II Stars, Davis, Philip A.G. (ed.).Google Scholar
Iben, I., 1981, Astrophys. J. 246, 278.CrossRefGoogle Scholar
Kippenhahn, R., Ruschenplatt, G., Thomas, H.-C., 1980, Astron. Astrophys. 91, 175.Google Scholar
Kippenhahn, R., Thomas, H.-C., Weigert, A., 1965, Z. f .Astrophys. 61, 241.Google Scholar
Kraft, R.P., 1972, Dudley Obs. Reports No. 4, Davis, Philip A.G. (ed.).Google Scholar
Kraft, R.P., 1981, personal communication.Google Scholar
Lauterborn, D., Refsdal, S., Weigert, A., 1971, Astron. Astrophys. 10, 97.Google Scholar
Maeder, A., 1975, Astron. Astrophys. 40, 303.Google Scholar
Matraka, B., Wassermann, C., Weigert, A., 1981, to appear in Astronomy & Astrophysics.Google Scholar
Paczyński, B., 1977, Astroph. J. 214, 812.Google Scholar
Paczyński, B., Tremaine, S.D., 1977, Astrophys. J. 216, 57.Google Scholar
Prialnik, D., Shaviv, G., Koretz, A., 1981, Astrophys. J. 247, 225.Google Scholar
Rose, W.K., 1966, Astrophys. J. 146, 838.Google Scholar
Schwarzschild, M., Härm, R., 1962, Astrophys. J. 136, 158.Google Scholar
Schwarzschild, M., Härm, R., 1965, Astrophys. J. 142, 855.Google Scholar
Schwarzschild, M., 1970, Quart. Journ. Roy. Astron. Soc. 11, 12.Google Scholar
Schwarzschild, M., Härm, R., 1970, Astrophys. J. 160, 341.Google Scholar
Sengbusch, K.v., 1967, Ph.D. thesis, Göttingen University.Google Scholar
Sugimoto, D., Nomoto, K., 1975, Pubi. Astr. Soc. Japan 27, 197.Google Scholar
Shaviv, G., Salpeter, E., 1973, Astrophys. J. 184, 191.Google Scholar
Sweigert, A.V., 1978, The HR-Diagramm, IAU Symp. No. 80 (1977),Philip, A.G.Davis and Hayes, D.S. (eds.), Reidel, p. 333.Google Scholar
Thomas, H.-C., 1967, Z. f. Astrophys. 67, 420.Google Scholar
Thomas, H.-C., 1970, Astrophys. Sp. Science 6, 400.Google Scholar
Tomkin, J., Lambert, D.L., Luck, R.E., 1975, Astrophys. J. 199, 436.CrossRefGoogle Scholar
Wassermann, C., 1979, Ph. D. Thesis, Hamburg University.Google Scholar
Weigert, A., 1975, Proc. 19th. Intern. Coll. Liège (1974), 355.Google Scholar
Wickett, A.J., 1977, Problñms of Stellar Convection, ed. Spiegel, E.A. and Zahn, J.P., in: Lecture Notes in Physics 71.Google Scholar
Wood, P.R., Zarro, D.M., 1981, Astrophys. J. 247, 247.Google Scholar