A model for clumpy giant molecular clouds with external ultraviolet heating

Details A model for clumpy giant molecular clouds with external ultraviolet heating A model for clumpy giant molecular clouds with external ultraviolet heating

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...356l..63t&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 356, June 20, 1990, p. L63-L66. Research supported by the Univers

Astronomy and Astrophysics

Astrophysics

46

Interstellar Matter, Molecular Clouds, Orion Nebula, Abundance, Astronomical Models, Carbon Monoxide, H Ii Regions, Temperature Gradients, Ultraviolet Radiation

Scientific paper

A model of clumpy molecular clouds based on that of Kwan and Sanders (1986) has been developed, in which a clump filling factor which is very low at the cloud surface and increases to about 1 at the cloud center allows the UV radiation from an H II region located at the surface to permeate the volume of the cloud and to create a temperature gradient and varying abundance of CO within each clump. The mode is in general agreement with the enhanced intensity of the (C-12)O J = 3-2 transition relative to the J = 1-0 line observed throughout the central 10-arcmin region of the Orion molecular cloud.

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