Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-29T17:33:24.355Z Has data issue: false hasContentIssue false
  • English
  • Français

Modelling PN Formation from Hydrodynamics and Radiation

Published online by Cambridge University Press:  07 August 2017

G. Mellema
G. Mellema*
Affiliation:
Sterrewacht Leiden, P.O. Box 9513, 2300 RA Leiden, The Netherlands

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.

The formation of planetary nebulae from the mass loss remnants of previous phases forms an interesting problem in both hydrodynamics and astrophysics. Not in the least because of the asphericity that most PNe show. The origin of this asphericity is still largely a mystery. Binarity is the most favoured explanation at the moment (Morris 1987)

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 369
Copyright
Copyright © Kluwer 1993 

References

Icke, V., Frank, A., Balick, B. (1992) A&A 253, 244.Google Scholar
Mellema, G., Eulderink, F., Icke, V. (1991) A&A 252, 719.Google Scholar
Morris, M. (1987) Publ. Astr. Soc Pac. 99, 1115.CrossRefGoogle Scholar
Soker, N. and Livio, M. (1989) ApJ 339, 268.CrossRefGoogle Scholar