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Stellar Evolution and the Planetary Nebula Formation Rate

Published online by Cambridge University Press:  19 July 2016

J. P. Phillips
J. P. Phillips*
Affiliation:
Physics Department, Queen Mary College, Mile End Road, London, El 4NS, England

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A knowledge of the formation rate of planetary nebulae is crucial to our understanding of a wide range of physical environments and processes, and as such has been fitfully investigated over the last forty or so years. The elemental composition of the interstellar medium, for instance, and in particular the seeding of the IS medium by CNO and s-process materials, turns out to be rather sensitively dependent upon the local rate of PN formation χ(PN) (Salpeter, 1978, Pottasch, 1984; Tinsley, 1978; and Wood et al, 1983). Similarly, and to varying degrees, the ionisation balance of the I.S. medium (cf. Pottasch, 1984; Salpeter, 1978), composition and number density of I.S. grains (Natta and Panagia, 1981), and ultimately the galactic star formation rate (cf. Miller and Scalo, 1979) can all (more or less directly) trace a dependency upon χ(PN). Finally, χ(PN) has proven historically important in establishing the evolutionary status of PN (cf. Abell and Goldreich, 1966), and is expected to be directly related to the rate of formation of white dwarfs, the death-rate of AGB-type stars (Mira variables, OH/IR sources), and the main-sequence turn-off rate in the mass range 2 ≲ M/M⊙ ≲ 10, some 1010 years ago.

Type
V. Origin of Planetaries
Information
Symposium - International Astronomical Union , Volume 131: Planetary Nebulae , 1989 , pp. 425 - 442
Copyright
Copyright © Kluwer 1989 

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