Hostname: page-component-7bb8b95d7b-qxsvm Total loading time: 0 Render date: 2024-09-12T05:16:47.310Z Has data issue: false hasContentIssue false
  • English
  • Français

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

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.

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