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Title:
Interstellar shock waves
Authors:
McKee, Christopher F.; Draine, Bruce T.
Affiliation:
AA(California, University, Berkeley), AB(Princeton University, NJ)
Publication:
Science (ISSN 0036-8075), vol. 252, April 19, 1991, p. 397-403.
Publication Date:
04/1991
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
COSMIC PLASMA, INTERSTELLAR MATTER, SHOCK WAVES, COMPUTERIZED SIMULATION, INTERSTELLAR MAGNETIC FIELDS, IONIZED GASES, MOLECULAR CLOUDS, SUPERNOVA REMNANTS
DOI:
10.1126/science.252.5004.397
Bibliographic Code:
1991Sci...252..397M

Abstract

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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