Cool C-shocks and high-velocity flows in molecular clouds

Details Cool C-shocks and high-velocity flows in molecular clouds Cool C-shocks and high-velocity flows in molecular clouds

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.242..495s&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 242, Feb. 1, 1990, p. 495-504.

Astronomy and Astrophysics

Astrophysics

53

Cooling Flows (Astrophysics), Interstellar Magnetic Fields, Molecular Clouds, Shock Waves, Stellar Evolution, Gas Ionization, Hydrogen, Mach Number, Subsonic Flow, Transition Flow

Scientific paper

C-shocks can be driven through dense clouds when the neutrals and magnetic field interact weakly due to a paucity of ions. A method is developed for calculating C-shock properties with the aim of interpreting the observed high-velocity molecular hydrogen. A high Mach number approximation, corresponding to low temperatures, is employed Under strong cooling conditions the flow is continuous even though a subsonic region may be present downstream. Analytic expressions for the maximum temperature, dissociation fraction, self-ionization level and J-shock transition are derived. This allows a wide range of velocities, densities, magnetic fields and ionization fractions to be explored and the parameter ranges for C-shocks to be displayed.

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