Interstellar shock waves

Details Interstellar shock waves Interstellar shock waves

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991sci...252..397m&link_type=abstract

Science (ISSN 0036-8075), vol. 252, April 19, 1991, p. 397-403.

Physics

33

Cosmic Plasma, Interstellar Matter, Shock Waves, Computerized Simulation, Interstellar Magnetic Fields, Ionized Gases, Molecular Clouds, Supernova Remnants

Scientific paper

The structure of the ISM is presently approached by way of the characteristics of its interstellar shock waves, which cause the tenuous plasma to radiate and thereby furnish diagnostics on both the ISM's physical conditions and the energy source producing the shock. The ISM plasma's degree of ionization, molecular content, small dust grains, and pervasive cosmic rays and magnetic field, all contribute to the variety of the structures of interstellar shocks. Increasingly powerful computer simulations are currently addressing such aspects of interstellar shock phenomenon behavior as collisionless heating of electrons, diffusive shock acceleration, and the stability of two-fluid MHD shocks.

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