Non-Equilibrium Thermal X-Ray Emission in Early Phase of Supernova Remnant

Details Non-Equilibrium Thermal X-Ray Emission in Early Phase of Supernova Remnant Non-Equilibrium Thermal X-Ray Emission in Early Phase of Supernova Remnant

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988pthph..80...83y&link_type=abstract

Progress of Theoretical Physics, Vol. 80, No. 1, pp. 83-95

Physics

3

Scientific paper

The X-ray emission from the interaction of the ejecta withcircumstellar matter (CSM) in the early phase of a supernova remnantis investigated. The electrons can be heated only through the Coulombcollisions with the ions behind the shock front. The electron and theion temperatures seem to be in non-equilibrium. Thus, in order toestimate the electron temperature and the X-ray luminosity, we studythe two-temperature model in the early phase. Self-similar solutionsare applied to describe the structure of the interaction region withshocked ejecta and shocked CSM. The average electron temperature andthe X-ray luminosity are estimated. They are expressed as a functionof the ratio of the progenitor's mass loss rate to the windvelocity. From an observed luminosity, we determine the ratio, whichcharacterizes the density of the CSM. As an example, the X-rayobservations for SN1987A in the range of 4-12 keV and 0.2-2.1 keV areanalyzed in terms of the simple analytic method. These observationsare explained as follows: When the ejecta have interacted withrelatively dense CSM, which had been formed in the stage of the redsupergiant before the blue supergiant, the X-ray emission from SN1987Ahas been detected. The soft X-ray emission below 1 keV will becomedominant in several decades after the explosion of SN1987A.

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