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On the Evolution of the Central Stars

Published online by Cambridge University Press:  14 August 2015

Willi Deinzer
Willi Deinzer*
Affiliation:
University of Heidelberg, Germany

Extract

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A most puzzling feature of the evolution of the central stars of planetary nebulae is their rapid contraction (O'Dell, 1963; Seaton, 1966); assuming homologous contraction, an enormous amount of gravitational energy is released therefore. For reasons of hydrostatic equilibrium a large part of this energy must be radiated away. As this does not show up in the luminosity of the central stars it must either leave them by some other means – e.g. neutrinos (Vila, 1966) – or it does not originate from the outset; in other words, the actual contraction must deviate strongly from the homologous way. I should like to discuss briefly the second possibility.

Type
Session VI – Origin and Evolution
Information
Symposium - International Astronomical Union , Volume 34: Planetary Nebulae , 1968 , pp. 428 - 430
Copyright
Copyright © Reidel 1968 

References

Baglin, A. (1966) private communication.Google Scholar
Deinzer, W. (1967) Z. Astrophys., 67, 342.Google Scholar
Hayashi, C., Hoshi, R., Sugimoto, D. (1962) Progress. theor. Phys., Suppl. 22.Google Scholar
O'Dell, C.R. (1963) Astrophys. J., 138, 67.Google Scholar
Schwarzschild, M. (1958) Structure and Evolution of the Stars, Princeton University Press. Princeton.Google Scholar
Seaton, M.J. (1966) Mon. Not. R. astr. Soc., 132, 113.Google Scholar
Vila, S.C. (1966) Astrophys. J., 146, 437.Google Scholar