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Pre-White Dwarf Evolution Through Planetary Nebulae

Published online by Cambridge University Press:  19 July 2016

Francesca D'antona  and
Italo Mazzitelli
Francesca D'antona
Affiliation:
Osservatorio Astronomico di Roma I-00040 Monte Porzio Italy
Italo Mazzitelli
Affiliation:
Istituto di Astrofisica Spaziale CNR C.P. 67 I-00044 Frascati Italy

Abstract

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In the present review we summarize the problems relative to the chemical composition of the inner and outer layers of white dwarfs as expected from stellar evolution. We point out that there is a contrast between standard predictions and the indications deriving from studies of white dwarfs, as “massive” hydrogen remnat layers seem not to be present on single white dwarfs. We discuss a previously neglected feature of stellar models in the phase of thermal pulses -which occurs when the outer hydrogen envelope becomes very small- by which the progenitors of low total mass may get rid of practically the whole hydrogen envelope during the final phases of asymptotic giant branch evolution. We finally propose a new global scheme for the pre-white dwarf evolution, which depends mainly on the initial progenitor mass.

Type
White Dwarfs
Information
Symposium - International Astronomical Union , Volume 145: Evolution of Stars: The Photospheric Abundance Connection , 1991 , pp. 399 - 409
Copyright
Copyright © Kluwer 1991 

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