On the energetics of high-velocity molecular flows

Details On the energetics of high-velocity molecular flows On the energetics of high-velocity molecular flows

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...299..191k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 1, 1985, p. 191-195. NSERC-supported research.

Astronomy and Astrophysics

Astrophysics

27

Molecular Clouds, Shock Waves, Stellar Envelopes, Stellar Evolution, Stellar Winds, Adiabatic Conditions, Momentum, Radial Velocity, Radiation Pressure, Stellar Models

Scientific paper

The paradox of excessive momentum observed in high-velocity flows near star-formation regions compared to the available photon momentum can be resolved by a model of adiabatic interaction between a stellar wind and the circumstellar molecular cloud. It is shown that the momentum of the swept-up material can be raised two orders of magnitude if the expansion of the swept-up shell is due to thermal pressure from a hot-shocked stellar wind. It is concluded that many of the observed properties of high-velocity flows are consistent with the hypothesis that the flows are driven by radiation pressure from the central star. It is suggested that the molecular cloud density distribution necessary to explain the high-velocity flow has a form of rho varies as r exp-3/2.

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