Interpretation of OH main line anomalies in interstellar clouds

Details Interpretation of OH main line anomalies in interstellar clouds Interpretation of OH main line anomalies in interstellar clouds

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....91..283b&link_type=abstract

Astronomy and Astrophysics, vol. 91, no. 3, Nov. 1980, p. 283-289.

Astronomy and Astrophysics

Astrophysics

18

Astronomical Models, Hydroxyl Emission, Interstellar Gas, Molecular Clouds, Electron Transitions, Gravitational Collapse, Hyperfine Structure, Velocity Distribution

Scientific paper

An excitation model is developed to interpret the nonthermal OH 18-cm main line emission observed in interstellar clouds. It is suggested that main line anomalies can be explained by far infrared overlap, resulting in a difference of about 1-3 K between the main line excitation temperatures. In a collapsing cloud, the 1667 MHz anomaly is found to appear for small collapse velocities (not greater than 1 km/s), whereas the 1665 MHz anomaly appears for higher velocities. The model is used to derive a set of physical parameters for the clouds in front of W 12 and 3C 123.

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