Author:
Faulkner D. J.,Wood P. R.
Abstract
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.
Publisher
Cambridge University Press (CUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
4 articles.
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