X-ray emission from supernova remnants MSH 14 - 63 and RCW 103

Details X-ray emission from supernova remnants MSH 14 - 63 and RCW 103 X-ray emission from supernova remnants MSH 14 - 63 and RCW 103

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...284..612n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 284, Sept. 15, 1984, p. 612-630.

Astronomy and Astrophysics

Astrophysics

40

High Temperature Plasmas, Supernova Remnants, X Ray Sources, Abundance, Emission Spectra, Nonequilibrium Ionization, Shock Waves, Stellar Evolution, X Ray Spectra

Scientific paper

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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