Interstellar OH Excitation

Details Interstellar OH Excitation Interstellar OH Excitation

Sep 1968

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1968natur.219.1138s&link_type=abstract

Nature, Volume 219, Issue 5159, pp. 1138-1139 (1968).

Physics

1

Scientific paper

THERE are now many observations of the 18 cm radio emission from the OH molecules located at the edges of HII regions1. The high intensities, narrow bandwidths, and strong polarizations associated with the emission have led to the conclusion that it is stimulated emission in a collimated beam. The problem of explaining the emission then reduces to a description of the mechanism by which the upper levels in the masering state of the molecule are overpopulated with respect to a thermal distribution. The first suggestions were that the stellar ultraviolet radiation provides a pumping mechanism2,3. It has been pointed out1, however, that the ultraviolet cannot pump at the rate (~1 cm-3 s-1) necessary for the brightest sources. As an alternative, Solomon4 has argued that because the OH is situated close to an HII region its lifetime must be short, so that overpopulation may be a result of the production mechanism. Here we discuss from this point of view a mechanism for the formation of OH recently proposed by us5.

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