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Title:
X-ray emission from supernova remnants MSH 14 - 63 and RCW 103
Authors:
Nugent, J. J.; Pravdo, S. H.; Garmire, G. P.; Becker, R. H.; Tuohy, I. R.; Winkler, P. F.
Affiliation:
AA(California Institute of Technology, Pasadena, CA), AB(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AC(Pennsylvania State University, University Park, PA), AD(Virginia Polytechnic Institute and State University, Blacksburg, VA), AE(Mount Stromlo and Siding Spring Observatories, Canberra, Australia), AF(Middlebury College, Middlebury, VT)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 284, Sept. 15, 1984, p. 612-630. (ApJ Homepage)
Publication Date:
09/1984
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
HIGH TEMPERATURE PLASMAS, SUPERNOVA REMNANTS, X RAY SOURCES, ABUNDANCE, EMISSION SPECTRA, NONEQUILIBRIUM IONIZATION, SHOCK WAVES, STELLAR EVOLUTION, X RAY SPECTRA
DOI:
10.1086/162444
Bibliographic Code:
1984ApJ...284..612N

Abstract

Electron-ion collisions, heavy element enrichment of emissions from reverse-shocked ejecta, abundances in the interstellar medium (ISM), the correspondence between the projected and measured age, ISM particle density, and distance, and classification factors for Type I or II supernovae are examined using a nonequilibrium ionization (NEI) model. The NEI model accounts for the absence of collisional ionization equilibrium and possibly thermal equilibrium between electrons and ions behind the shock fronts, and describes the emission spectra from ejecta and the shocked ISM. When applied to data from the SNR MSH 14 - 63 a non-Coulomb, ion-electron interaction is obtained that is consistent with a shocked ISM. For the SNR RCW 103, however, the processes behind the shock front are not discernable, although the elemental abundances will have solar values if the interactions are non-Coulomb. The age of RCW 103 must be approximated from physical data, as Chinese astronomers would not have been able to see the event from their position on earth two millenia ago.

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