Abstract: Shocks are ubiquitous in the interstellar and intergalactic media, where their chemical and radiative signatures reveal the physical conditions in which they arise. Detailed astrochemical models of shocks at all velocities are necessary to understand the physics of many environments including protostellar outflows, supernova remnants, and galactic outflows. We present an accurate treatment of the self-generated UV radiation in intermediate velocity, stationary, weakly magnetised, J-type, molecular shocks. Shock solutions computed with the Paris...
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Topics: 
Astrophysics
Computational physics