OH 1720 MHz Masers in Supernova Remnants --- C-Shock Indicators

Abstract

Recent observations show that the OH 1720 MHz maser is a powerful probe of the shocked region where a supernova remnant strikes a molecular cloud. We perform a thorough study of the pumping of this maser and find tight constraints on the physical conditions needed for its production. The presence of the maser implies moderate temperatures (50 -- 125 K) and densities ($\sim 10^{5}c{m}^{-3}$), and OH column densities of order $10^{16}c{m}^{-2}$. We show that these conditions can exist only if the shocks are of C-type. J-shocks fail by such a wide margin that the presence of this maser could become the most powerful indicator of C-shocks. These conditions also mean that the 1720 MHz maser will be inherently weak compared to the other ground state OH masers. All the model predictions are in good agreement with the observations.

16 pages, 5 Postscript figures (included), uses aaspp4.sty. To appear in the Astrophysical Journal

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