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Carbon Stars as Planetary Nebula Progenitors

Published online by Cambridge University Press:  19 July 2016

G. R. Knapp
G. R. Knapp*
Affiliation:
Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, U.S.A.

Abstract

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Molecular line observations show that some planetary nebulae are still only partially ionized and are surrounded by the remains of the mass loss envelope shed by the preceding AGB star. The mass loss rates and outflow velocities of these envelopes are similar to those of the cool winds from luminous AGB stars. Both the kinematics of carbon stars and observations of the molecular envelopes around young planetaries show that the carbon star progenitors have a wide range of ages and of mass loss rates. There is increasing evidence that a significant fraction of AGB stars are carbon stars and that these provide a substantial contribution to the total mass returned to the interstellar medium.

Type
V. Origin of Planetaries
Information
Symposium - International Astronomical Union , Volume 131: Planetary Nebulae , 1989 , pp. 381 - 390
Copyright
Copyright © Kluwer 1989 

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