Shapes of planetary nebulae

Details Shapes of planetary nebulae Shapes of planetary nebulae

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.212..837k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 212, Feb. 15, 1985, p. 837-850. Research supported by t

Astronomy and Astrophysics

Astronomy

163

Planetary Nebulae, Stellar Winds, Angular Momentum, Gas Pressure, Stellar Mass Ejection, Stellar Models

Scientific paper

The formation of planetary nebulae can be discussed in terms of an interacting stellar winds model, in which the slow wind from the progenitor star is later overtaken by the fast wind from the central star. As a result of the interaction the inner region of the slow wind is compressed into a dense shell. The consequences for the model of a red-giant wind in which the mass-loss rate is enhanced towards the equator are investigated. The resulting shell is elongated in the direction of the poles. The treatment is simmplified, in that the finite temperature of the compressed shell is neglected. Consequently, the cusps which are sometimes found at the equator are, in reality, regions of high density.

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