The motion and distribution of the vibrationally excited H2 in the Orion molecular cloud

Details The motion and distribution of the vibrationally excited H2 in the Orion molecular cloud The motion and distribution of the vibrationally excited H2 in the Orion molecular cloud

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...253..154n&link_type=abstract

Astrophysical Journal, Part 1, vol. 253, Feb. 1, 1982, p. 154-166. NSF-NASA-supported research.

Astronomy and Astrophysics

Astrophysics

80

Hydrogen, Interstellar Gas, Molecular Clouds, Molecular Excitation, Orion Nebula, Vibrational Spectra, Radial Velocity, Shock Waves

Scientific paper

Observations of the v=1-0 S(1) and S(0), and v=2-1 S(1) emission lines of H2 in the Orion molecular cloud are presented, showing that the emission region has an approximately circular symmetry, which may be divided into a central and a peripheral region. The emission lines in the central region have a large range of velocities, and predominantly occur at the negative velocities of 0 to -100 km/sec, while those at the periphery are symmetric. The brightness of the peak emission is generally higher at positions in the periphery than in the central region. These results lead to a model of H2 line emission in which there is gas undergoing radial expansion at velocities of up to about 100 km/sec within a region of some 2.5 x 10 to the 17th cm in diameter around the cluster of IR sources. A substantial part of the H2 line emission comes from the outside boundary of this expansion region, where the flow collides with the gas in the molecular cloud.

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