Non-Thermal Radiative Cooling in Continuous Shocks

Details Non-Thermal Radiative Cooling in Continuous Shocks Non-Thermal Radiative Cooling in Continuous Shocks

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995iraj...22...33o&link_type=abstract

Irish Astronomical Journal, 1995, 22(1), 33

Astronomy and Astrophysics

Astronomy

Scientific paper

Energy moving through molecular clouds produces shocks which have been widely studied. Current models, based on magnetohydrodynamic (MHD) principles, fail to explain the observed high velocities with which these shocks can move without dissociating molecular hydrogen as well as the emission spectra, especially for diffuse clouds. The use of MHD techniques requires local thermodynamic equilibrium in the medium, and in molecular clouds this is often not a good assumption. By using a Monte-Carlo particle simulation of the system it can be seen that the radiation differs significantly from current models. This increase in radiation should allow higher-velocity shocks and bring theory more in to line with experiment.

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