The structure of radiation from shock waves in the interstellar medium

Details The structure of radiation from shock waves in the interstellar medium The structure of radiation from shock waves in the interstellar medium

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64..509b&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, May-June 1987, p. 509-519. In Russian.

Statistics

Computation

Computational Astrophysics, Interstellar Space, Plasma Cooling, Plasma Temperature, Radiation Distribution, Shock Fronts, Balmer Series, Emission Spectra, Flow Characteristics, Line Spectra, Shock Waves, Supernova Remnants

Scientific paper

The system of equations describing nonstationary cooling of two-temperature plasma behind the shock wave front is presented. The physical processes inside the front are discussed. The flow motion is converted into heat energy of heavy particles (ions and atoms) in the wide region of flow parameters, while electrons are heated mainly by comparatively weak adiabatic compression. The calculations of emission-line absolute intensities, Balmer decrement, and stratification of hydrogen, nitrogen, oxygen, and sulphur line intensities are compared with the available supernova remnant observations.

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