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Evolutionary Calculations for Planetary Nebula Nuclei with Continuing Mass Loss and Realistic Starting Conditions

Published online by Cambridge University Press:  25 April 2016

D. J. Faulkner  and
P. R. Wood
D. J. Faulkner
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
P. R. Wood
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
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Extract

The mechanism by which planetary nebula (PN) shells are ejected is still subject to considerable uncertainty. It is generally assumed that the precursors of these objects are low mass (M< 5 M⊙) asymptotic giant branch (AGB) stars, and that the nucleus of a planetary nebula (NPN) is undergoing a final gravitational contraction to the white dwarf state. The shell consists of some or all of the remaining unburnt (though not necessarily uncontaminated), hydrogen-rich material out of which the star was originally formed.

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Contributions
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Publications of the Astronomical Society of Australia , Volume 5 , Issue 4 , 1984 , pp. 543 - 546
Copyright
Copyright © Astronomical Society of Australia 1984

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