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The Influence of Equilibration on the X-ray Intensity of Sedov Models

Published online by Cambridge University Press:  12 April 2016

D. Jerius  and
R.G. Teske
D. Jerius
Affiliation:
Department of Astronomy, University of Michigan, Ann Arbor, Michigan
R.G. Teske
Affiliation:
Department of Astronomy, University of Michigan, Ann Arbor, Michigan

Abstract

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We have synthesized a set of SNR X-ray and coronal iron surface brightness profiles to determine observational constraints to help distinguish how the remnants’ ion-electron energy equilibration time-scales compare to their ionization time-scales. The profiles are based on Sedov-Taylor blast wave models under the two scenarios (1) equal Tion and Te or (2) Coulomb equilibration of Te and Tion. Resultant spectra were convolved with Einstein HRI and IPC sensitivity curves to simulate satellite observations of actual remnants.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 101: Supernova Remnants and the Interstellar Medium , 1988 , pp. 145 - 148
Copyright
Copyright © Cambridge University Press 1988

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