Interpreting the Molecular Hydrogen Emission
نویسندگان
چکیده
Intense emission lines of near{IR molecular hydrogen are excited in OMC{1 by shocks, as outtowing gas from the star forming core interacts with the surrounding molecular cloud. These have been studied in OMC{1 in far greater detail than in any other astronomical source. They provide both a picture of the energetic activity associated with massive star formation, and stringent constraints on models for shock emission. They also ooers insights into the way winds interact with, and sweep up, interstellar gas. This review discusses the current state of observations of molecular hydrogen line emission from OMC{1, and its interpretation in the context of shock models and magnetohydrodynamical instabilities.
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تاریخ انتشار 2007