Stellar winds in H II regions - Unstable waves in ionized shells

Details Stellar winds in H II regions - Unstable waves in ionized shells Stellar winds in H II regions - Unstable waves in ionized shells

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.235.1011b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 235, Dec. 15, 1988, p. 1011-1023. Research supported by

Computer Science

Sound

17

Hot Stars, Hydrogen Clouds, Hydrogen Ions, Magnetohydrodynamic Stability, Planetary Nebulae, Stellar Winds, Shock Heating, Sound Waves

Scientific paper

The authors investigate in some detail the nature of acoustic disturbances in an ionized shell which is held under pressure by a shocked stellar wind, and surrounds a hot star such as an OB star or the nucleus of a planetary nebula. They find that for a large range of wavenumbers such waves can grow to finite amplitude in a time that is of the order of the sound crossing time for the H II layer, and therefore short compared with the dynamical time-scale of the nebula as a whole. An important consequence is that mixing will then occur between the hot shocked gas from the stellar wind and the cooler gas in the H II region.

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