Shapes of wind driven circumstellar shells

Details Shapes of wind driven circumstellar shells Shapes of wind driven circumstellar shells

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984stfm.work..129k&link_type=abstract

In Royal Observatory Star Formation Workshop p 129-132 (SEE N85-12809 03-88)

Computer Science

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Stellar Envelopes, Stellar Evolution, Stellar Models, Stellar Winds, Interstellar Gas, Mass Distribution, Planetary Nebulae, Rotating Spheres

Scientific paper

A star formation model which allows for departures from spherical symmetry is proposed. The asphericity results from anisotropy in the distribution of mass loss from the progenitor star of a planetary nebula. Ambient gas of the slow wind is swept into a cool shell and driven outwards; fast wind gas is shocked, and forms a bubble of hot gas enclosed by this shell. The expansion speed of the cool shell is slow compared with the sound speed in the hot shocked wind. Therefore the pressure of the hot gas is (almost) uniform within the bubble. But there is more mass to push outwards in those directions where the ambient gas is denser, so the shell expands more slowly there, i.e., the shell is no longer spherical.

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