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Planetary nebulae in the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

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

Abstract

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We present a simple two-wind model for the evolution of the Magellanic Cloud planetary nebulae (PN) which reproduces the observed density / radius / ionised mass relationships, and serves to define the geometrical relationship between the ionised nebula and the star. From self-consistent photoionisation modelling of 78 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 masses generally between 0.55 and 0.7 M⊙. Type I PN have more massive precursors, and show clear evidence for the Third dredge-up episode and for the dredge-up of ON processed material. The expansion velocity of the nebula is closely correlated with the position of the central star on the H-R Diagram, proving that the nebula undergoes continuous acceleration. Excluding Type I PN, the mean abundances derived for the LMC and the SMC agree with those derived from H II regions and evolved, radiative SNR.

Type
Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 299 - 306
Copyright
Copyright © Kluwer 1991 

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