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Stellar evolution in the Magellanic Clouds from studies of planetary nebulae

Published online by Cambridge University Press:  07 August 2017

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 CB3 0EZ

Extract

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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 40 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
Poster Papers
Information
Symposium - International Astronomical Union , Volume 149: The Stellar populations of Galaxies , 1992 , pp. 502
Copyright
Copyright © Kluwer 

References

Monk, D. J., Barlow, M. J. & Clegg, R. E. S., 1988. Mon. not. R. astr. Soc. , 234, 583.Google Scholar
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Walton, N.A., Barlow, M.J., Monk, D.J., Clegg, R.E.S., 1991. Mon. not. R. astr. Soc. , submitted.Google Scholar