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Thermal Pulses and the Formation of Planetary Nebula Shells

Published online by Cambridge University Press:  19 July 2016

Alvio Renzini
Alvio Renzini*
Affiliation:
Dipartimento di Astronomia, Università di Bologna, Bologna, Italy

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Over the past decade a comprehensive, semiquantitative theoretical scenario for the final evolutionary stages of low and intermediate mass stars has been progressively elaborated and refined. It concerns the envelope ejection terminating the Asymptotic Giant Branch (AGB) phase, the AGB to Planetary Nebula (PN) transition, the fading and possible rejuvenation of PN nuclei, the formation processes of hydrogen-deficient stars, and the final production of white dwarfs (WD) of the DA and non-DA varieties (Renzini 1979, 1981a, 1981b, 1982, 1983, Iben & Renzini 1983, Iben et al. 1983, Iben 1984, 1985, 1987, Iben & Tutukov 1984, Iben & MacDonald 1985, 1986). In developing this scenario several important results of stellar evolution and hydrodynamical calculations have been incorporated, including in particular those of Paczynski (1971), Wood (1974), Härm & Schwarzschild (1975), Schönberner (1979, 1983), and Tuchman, Sack & Barkat (1979).

Type
V. Origin of Planetaries
Information
Symposium - International Astronomical Union , Volume 131: Planetary Nebulae , 1989 , pp. 391 - 400
Copyright
Copyright © Kluwer 1989 

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