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Thermal and Density Structures and Elemental Abundances in the Bipolar PN Mz 3

Published online by Cambridge University Press:  26 May 2016

Y. Zhang  and
X.-W. Liu
Y. Zhang
Affiliation:
1 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China
X.-W. Liu
Affiliation:
2Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

Extract

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Mz 3 is a young bipolar planetary nebula (PN) with lobes extending over ~ 50 arcsec on the sky. It consists of a bright core, two approximately spherical bipolar lobes and two outer large filamentary bipolar nebulae. The salient features of Mz 3 are more easily studied than other bipolar nebula because of its large angular extent. It is very bright in the far-infrared. There is an extended shell of warm dust surrounding the central star. And the bipolar lobes are filled with hot ionized gas. Cohen et al. (1978) found that Mz 3 is He-rich. Based on the LWS observations of the far-IR fine-structure lines, Liu et al. (2001) derived a high N/O ratio in Mz 3 and identified the bipolar nebula as a Type-I PN.

Type
Part VI: The Ionized Gas in Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 377 - 378
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Cohen, M., Kunkel, W., Lasker, B. M., et al. 1978, ApJ, 221, 151 Google Scholar
Liu, X.-W., Barlow, M. J., Cohen, , et al. 2001, MNRAS, 323, 343 CrossRefGoogle Scholar
Schmeja, S., & Kimeswenger, S., 2001, astro-ph/0108331 Google Scholar