Collisional Pumping of OH Masers near Supernova Remnants

Abstract

The collisional pumping of OH masers in non-dissociative C-type shocks near supernova remnants is considered. The emergence of maser emission in OH lines is investigated for various shock parameters - the shock speed, the preshock gas density, the cosmic-ray ionization rate, and the magnetic field strength. The largest optical depth in the 1720 MHz line is reached at high gas ionization rates $\zeta \ge 10^{-15}$ s${}^{-1}$, an initial density $n_{\mathrm{H},0}\le 2\times 10^4$ cm${}^{-3}$, and a shock speed $u_{\mathrm{s}}\ge 20$ km s${}^{-1}$. According to our calculations, there is also a level population inversion for the 6049 and 4765 MHz transitions of excited OH rotational states. However, the optical depth in these lines is small for all of the investigated shock parameters, which explains the non-detection of maser emission in these lines in supernova remnants.

17 pages, 4 figures

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Cited by in corpus (2)

• Modelling cosmic masers in C-type shock waves -- the coexistence of Class I CH3OH and 1720 MHz OH masers
• Collisional Pumping of H${}_2$O and CH${}_3$OH Masers in C-Type Shock Waves