Non-Equilibrium Thermal X-Ray Emission in Early Phase of Supernova Remnant : Astrophysics and Relativity

概要

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The X-ray emission from the interaction of the ejecta with circumstellar matter (CSM) in the early phase of a supernova remnant is investigated. The electrons can be heated only through the Coulomb collisions with the ions behind the shock front. The electron and the ion temperatures seem to be in non-equilibrium. Thus, in order to estimate the electron temperature and the X-ray luminosity, we study the two-temperature model in the early phase. Self-similar solutions are applied to describe the structure of the interaction region with shocked ejecta and shocked CSM. The average electron temperature and the X-ray luminosity are estimated. They are expressed as a function of the ratio of the progenitor's mass loss rate to the wind velocity. From an observed luminosity, we determine the ratio, which characterizes the density of the CSM. As an example, the X-ray observations for SN1987A in the range of 4-12 keV and 0.2-2.1 keV are analyzed in terms of the simple analytic method. These observations are explained as follows: When the ejecta have interacted with relatively dense CSM, which had been formed in the stage of the red supergiant before the blue supergiant, the X-ray emission from SN1987A has been detected. The soft X-ray emission below 1 keV will become dominant in several decades after the explosion of SN1987A.
理論物理学刊行会の論文
1988-07-25