A planetary nebula consists mainly of gas ejected slowly by a red giant. Its dynamics is dominated by the hot central star which is left behind later. In particular a fast wind from this star forms a bubble of hot gas which fills the inner part of the nebula and pushes the envelope into a shell. This shell remains only partly ionized for a considerable time. Its non-ionized part is subject to a Rayleigh-Taylor instability, and is expected to break up into fragments which remain behind in the HII part of the nebula.
CITATION STYLE
Kahn, F. D. (1983). Fast Winds in Planetary Nebulae. Symposium - International Astronomical Union, 103, 305–316. https://doi.org/10.1017/s0074180900093815
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