Hostname: page-component-84b7d79bbc-x5cpj Total loading time: 0 Render date: 2024-07-27T21:32:16.499Z Has data issue: false hasContentIssue false
  • English
  • Français

Theory of Evolution of Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  22 September 2016

B. Paczyński
B. Paczyński*
Affiliation:
Princeton University Observatory and N. Copernicus Astronomical Center, Polish Academy of Sciences

Abstract

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.

Young central stars of planetary nebulae burn hydrogen and helium in the shell sources. Within less than 104 years nuclear fuel is exhausted and old central stars cool off at almost constant radius to the white dwarf stage.

Young, i.e., luminous central stars should follow complicated loops on the H-R diagram as a result of helium shell flashes. FG Sagittae is the example. This should be a typical behaviour and a systematic search for light variations on a time scale of years or decades among other luminous entral stars should be undertaken. Because of rapid evolution of their nuclei many planetary nebulae may be far from the ionization equilibrium. This should be taken into account when the effective temperature and bolometric luminosity of the central stars are estimated.

Type
Session IV: The Central Stars of Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 76: Planetary Nebulae , 1978 , pp. 201 - 205
Copyright
Copyright © Reidel 1978 

References

Abell, G. and Goldreich, P.: 1966, Publ. A.S.P., 78, 232.CrossRefGoogle Scholar
Christy-Sackmann, I.-J., and Despain, K.H.: 1974, Ap.J., 189, 523.Google Scholar
Harm, R. and Schwarzschild, M.: 1975, Ap.J., 200, 324.Google Scholar
Herbig, G.H. and Boyarchuk, A.A.: 1968, Ap.J., 153, 397.CrossRefGoogle Scholar
Iben, I. Jr.: 1974, Ann. Rev. Astron. Ap., 12, 215.CrossRefGoogle Scholar
Krzeminski, W., Priedhorsky, W. and Miller, J.: 1976, I.A.U. Circ. No. 2974.Google Scholar
Mendez, R.H. and Niemela, V.S.: 1977, M.N.R.A.S., 178, 409.CrossRefGoogle Scholar
O'Dell, C.R.: 1963, Ap.J., 138, 67.CrossRefGoogle Scholar
O'Dell, C.R.: 1968, I.A.U. Symposium No. 34. Planetary Nebulae (Dordrecht-Holland: D. Reidel Publ. Co.), p. 369.Google Scholar
Paczyński, B.: 1970, Acta Astron., 20, 47.Google Scholar
Paczyński, B.: 1971, Acta Astron., 21, 417.Google Scholar
Paczyński, B.: 1975, Ap.J., 202, 558.CrossRefGoogle Scholar
Paczyński, B.: 1976, I.A.U. Symposium No. 73: Structure and Evolution of Close Binary Systems (Dordrecht-Holland: D. Reidel Publ. Co.), p. 75.CrossRefGoogle Scholar
Rose, W.K. and Smith, R.L.: 1970, Ap.J., 159, 903.CrossRefGoogle Scholar
Salpeter, E.E.: 1971, Ann. Rev. Astron. Ap., 9, 127.CrossRefGoogle Scholar
Schwarzschild, M. and Harm, R.: 1965, Ap.J., 142, 855.CrossRefGoogle Scholar
Seaton, M.: 1966, M.N.R.A.S., 132, 113.CrossRefGoogle Scholar
Shklovsky, I.: 1956, Astron. Zh., 33, 315.Google Scholar
Smith, L.S.: 1968, Wolf-Rayet Stars (N.B.S. Special Publ., Gebbie, K.B. and Thomas, R.N., Eds.), p. 21.Google Scholar
Smith, L.S.: 1973, I.A-U. Symposium No. 49: Wolf-Rayet and High Temperature Stars (Dordrecht-Holland: D. Reidel Publ. Co.), p. 126.Google Scholar