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Angular Diameters of Magellanic Cloud Planetary Nebulae Obtained using Speckle Interferometry

Published online by Cambridge University Press:  25 April 2016

P. R. Wood ,
M. S. Bessell  and
M. A. Dopita
P. R. Wood
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
M. S. Bessell
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
M. A. Dopita
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National University
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Abstract

Angular diameters of Magellanic Cloud planetary nebulae obtained using speckle interferometry on the AAT are presented. The mass of ionized gas in each nebula is derived from the angular diameter and published Hβ line fluxes; the derived masses range from 0.005M⊙ to 0.19M⊙, with a mean value of 0.08M⊙. All the planetary nebulae observed are relatively small (diameter ≲0.13pc), young (age ≲ 2500 years), bright and dense. They are therefore almost certainly only partially ionized, so that the masses derived for the ionized parts of the nebula are lower limits to the total nebula mass.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 6 , Issue 1 , 1985 , pp. 54 - 55
Copyright
Copyright © Astronomical Society of Australia 1985

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References

Acker, A., 1978, Astron. Astrophys. Suppl., 33, 367.Google Scholar
Aller, L. H., 1983, Astrophys. J., 273, 590.CrossRefGoogle Scholar
Cahn, J. H., and Kaler, J. B., 1971, Astrophys. J. Suppl., 22, 319.CrossRefGoogle Scholar
Cudworth, K. M., 1974, Astron. J., 79, 1384.CrossRefGoogle Scholar
Daub, C. T., 1982, Astrophys. J., 260, 612.CrossRefGoogle Scholar
Dopita, M. A., Ford, H. C., Lawrence, C. J., and Webster, B. L., 1985, Astrophys. J., in press.Google Scholar
Dopita, M. A., Ford, H. C., and Webster, B. L., 1985a, Astrophys J., in press.Google Scholar
Dopita, M. A., Ford, H. C., and Webster, B. L., 1985b, private communication.Google Scholar
Iben, I., 1984, Astrophys. J., 277, 333.CrossRefGoogle Scholar
Morgan, D. H., 1984, Mon. Not. R. Astron. Soc., 208, 633.Google Scholar
Pottasch, S. R., 1983, in IAU Symp. No. 103, Planetary Nebulae, ed. Flower, D. R. (Dordrecht: Reidel), p. 391.Google Scholar
Sanduleak, N., MacConnell, D. J., and Philips, A. G. D., 1978 Pubi Astron. Soc. Pacific, 90, 621.CrossRefGoogle Scholar
Seaton, M. J., 1966, Mon. Not. R. Astron. Soc., 132, 113.CrossRefGoogle Scholar
Webster, B. L., 1969, Mon. Not. R. Astron. Soc., 143, 79.CrossRefGoogle Scholar
Webster, B. L., 1976, Mon. Not. R. Astron. Soc., 174, 513.CrossRefGoogle Scholar
Wood, P. R., 1985, Proc. Astron. Soc. Aust., 6, 118.Google Scholar
Wood, P. R., and Faulkner, D. J., 1985, Astrophys. J., submitted.Google Scholar