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The Evolution of the Planetary Nebulae in the Magellanic Clouds and the Galactic Bulge

Published online by Cambridge University Press:  07 August 2017

M.A. Dopita
M.A. Dopita*
Affiliation:
Mt. Stromlo and Siding Spring Observatories, Institute of Advanced Studies, The Australian National University

Abstract

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From self-consistent photoionisation modelling of 147 Magellanic Cloud PN, we have constructed the H-R Diagram for the central stars, and have derived both the chemical abundances and the nebular parameters. We find that the central stars have core masses generally between 0.55 and 0.7 M⊙, and find strong evidence to support the model that they leave the AGB as helium-burning stars following the final shell flash. Type I PN have more massive cores, up to near the Schwartzschild limit, and show clear evidence for the Third dredge-up episode. From HST images, younger PN are very compact. The expansion velocity of the nebula is closely correlated with the position of the central star on the H-R Diagram.

Type
V. Planetary Nebulae Connection: Evolution to White Dwarfs
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 433 - 441
Copyright
Copyright © Kluwer 1993 

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