Abstract
Abstract The temperatures of the plasma in supernova remnants (SNRs) are initially very low just after the shock heating. The electron temperature (kTe) increases quickly by Coulomb interaction, and then the energetic electrons gradually ionize atoms to increase the ionization temperature (kTi). The observational fact is that most young and middle-to-old SNRs have lower kTi than kTe after the shock heating. The temperature evolution in shell-like SNRs has been explained by this ionizing plasma (IP) scenario. On the other hand, in the last decade, a significant fraction of mixed-morphology SNRs was found to exhibit a recombining plasma (RP) with higher kTi than kTe. The origin and the evolution mechanism of RP SNRs have been puzzling. To address this puzzle, this paper presents kTe and kTi profiles using follow-up Suzaku observations, and then proposes a new scenario for the temperature and morphology evolution in IP and RP SNRs.
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