Hostname: page-component-586b7cd67f-t8hqh Total loading time: 0 Render date: 2024-11-27T00:39:38.397Z Has data issue: false hasContentIssue false
  • English
  • Français

Abundances and nebular and central star masses for Magellanic Cloud planetary nebulae

Published online by Cambridge University Press:  19 July 2016

N. A. Walton ,
M. J. Barlow ,
D. J. Monk  and
R.E.S. Clegg
N. A. Walton
Affiliation:
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT
M. J. Barlow
Affiliation:
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT
D. J. Monk
Affiliation:
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT
R.E.S. Clegg
Affiliation:
Royal Greenwich Observatory, Madingley Road, Cambridge CBS OEZ

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the results of a spectroscopic study of planetary nebulae (PN) in the Magellanic Clouds. The optical survey of He, N, O, and Ne abundances by Monk et al. (1988) has been updated by higher S/N AAT optical data. In addition, carbon and other elemental abundances have been derived from the IUE spectra of 38 PN. Ionized nebular masses have been derived for 80 PN. The ionised mass versus nebular electron density plot shows that planetary nebulae become optically thin when their electron densities drop below 4500 cm--3. Below this density, the mean nebular hydrogen mass found for non-Type I PN is 0.22±0.08 M⊙. Using Zanstra and energy-balance methods, the mean central star mass found for 14 SMC and LMC PN is 0.59±0.02 M⊙.

Type
Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 334 - 336
Copyright
Copyright © Kluwer 1991 

References

Barlow, M. J., 1990. These Proceedings.Google Scholar
Monk, D. J., Barlow, M. J. & Clegg, R. E. S., 1988. Mon. not. R. astr. Soc. , 234, 583.CrossRefGoogle Scholar