Atomic hydrogen in the Orion star-forming region

Details Atomic hydrogen in the Orion star-forming region Atomic hydrogen in the Orion star-forming region

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989aj.....98.2203c&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 98, Dec. 1989, p. 2203-2209, 2375, 2376. Research supported by the Mellon Foundation

Astronomy and Astrophysics

Astronomy

37

Hydrogen Atoms, Molecular Clouds, Orion Nebula, Star Formation, Electron Transitions, Emission Spectra, Photodissociation, Stellar Luminosity

Scientific paper

A large-scale survey of atomic hydrogen in Orion reveals low-density material with a total mass comparable to that in dense molecular clouds. The atomic gas is sufficiently dense that it can shield the molecular material from photodissociative radiation and provide a pressure link to the low-density intercloud medium. An excess of H I emission comes from photodissociation fronts near the bright stars and from a giant shell in the Orion Belt region. This shell may have caused the apparent bifurcation between the Orion A and B clouds, and the associated pressures may have induced peculiar motions and star formation in NGC 2023 and 2024.

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