Fast Molecular Hydrogen from Time-Dependent Shocks

Details Fast Molecular Hydrogen from Time-Dependent Shocks Fast Molecular Hydrogen from Time-Dependent Shocks

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxac..15..131l&link_type=abstract

Winds, Bubbles, and Explosions: a conference to honor John Dyson, Pátzcuaro, Michoacán, México, September 9-13, 2002 (Eds. S. J.

Astronomy and Astrophysics

Astronomy

2

Ism: Jets And Outflows, Stars: Mass Loss, Stars: Pre-Main Sequence

Scientific paper

It is a well known but puzzling result that zones within star-formation regions sometimes show molecular hydrogen emission at very high ( ~ 100km/s) velocities. These kinds of observations are somewhat difficult to explain because high-speed, non-magnetized, J-type shock waves mostly dissociate the molecules present in the preshock medium, and therefore produce almost no H[2] emission.
We present models in which a shock wave gradually accelerates. We find that such shock waves are indeed able to accelerate significant masses of molecular material to velocities of ~ 100km/s, and are a plausible explanation for the widely observed, high velocity H[2] emission.

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