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Chemistry in Interstellar Hydroxyl Maser Regions

Published online by Cambridge University Press:  04 August 2017

T. W. Hartquist
T. W. Hartquist*
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, Institut, für extraterrestrische Physik, 8046 Garching, F.R.G., Astronomy Program, University of Maryland, College Park, Maryland 20742, U.S.A.

Abstract

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The pumping of the upper levels of the 2π3/2 J=3/2 state of OH at sufficient rates to account for the observed strengths of interstellar hydroxyl masers requires that OH contains a substantial fraction of the oxygen. Shocks have been suggested as the sites of the OH production, but a better understanding of OH photodissociation and observations of hydroxyl maser kinematics have led to the realization that the original hydroxyl maser shock model must be revised. the possibility that interstellar hydroxyl masers occur in dense molecular photodissociation zones, heated by photoabsorption and perhaps by ion-neutral friction in the magnetic precursor of a shock, is considered. Possible infrared line emission from interstellar hydroxyl maser regions is mentioned.

Type
Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 120: Astrochemistry , 1987 , pp. 297 - 302
Copyright
Copyright © Reidel 1987 

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