The formation of discrete high velocity molecular features

Details The formation of discrete high velocity molecular features The formation of discrete high velocity molecular features

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.228..957h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 228, Oct. 15, 1987, p. 957-961. Research supported by t

Astronomy and Astrophysics

Astronomy

24

Hydrogen, Molecular Clouds, Water Masers

Scientific paper

Clumps embedded in a flowing diffuse medium will be dissipated before ram pressure accelerates them substantially. Molecular hydrogen can be accelerated to high speeds by passing through a slow shock leading a shell at the edge of a wind-driven bubble if the density in the ambient medium drops rapidly enough to allow the shell to accelerate subsequently. The shell will be subject to the Rayleigh-Taylor instability which will drive transonic turbulence but will not initiate the formation of fragments having large density contrasts until the shell reaches sufficient speeds to become thermally unstable. The existence of high velocity discrete features in and the magnitude of the linewidth of the H2 emission from CRL 618 are explained with this acceleration mechanism. High velocity water masers may be formed in a similar fashion, but not Herbig-Haro objects.

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