Influence of the equilibration process in supernova remnant shocks on their X-ray and coronal iron surface brightnesses

Details Influence of the equilibration process in supernova remnant shocks on their X-ray and coronal iron surface brightnesses Influence of the equilibration process in supernova remnant shocks on their X-ray and coronal iron surface brightnesses

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apjs...66...99j&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 66, Feb. 1988, p. 99-123.

Astronomy and Astrophysics

Astronomy

5

Metallicity, Stellar Coronas, Stellar Luminosity, Supernova Remnants, X Ray Astronomy, Iron, Stellar Models

Scientific paper

SNR model computation results have been obtained which indicate that the radial distribution of soft X-ray and forbidden coronal Fe surface brightnesses in adiabatic, middle-aged SNRs can be used as a basis of discrimination for whether the equilibration time is short or long, by comparison with the ionization time-scale. These models are based on a grid of Sedov-Taylor models with time-dependent, nonequilibrium collisional ionization of 13 chemical elements; the two extreme equilibration conditions assumed are T(ion) = T(e) and a Coulomb equilibration of ion and electron temperatures. The models are compared with data taken from X-ray images of the Cygnus Loop and Puppis A.

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