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T.G. Pannuti, J. Rho (Spitzer Science Center/JPL/Caltech)
Mixed-morphology supernova remnants (SNRs) are a new class of SNR which are characterized by a shell-like radio morphology combined with a center-filled X-ray morphology with a thermal spectrum. Several models have been proposed to explain the origin of this unique combination of X-ray and radio morphologies for these SNRs, but a comprehensive understanding of these sources remains elusive. To help elucidate the properties of these sources, we are performing both spatial and spectral analyses of X-ray emission from a sample of known mixed-morphology SNRs using archived ASCA observations. To illustrate this research, we will present spatial and spectral results for two known mixed-morphology SNRs, HB21 and CTB 1. HB21 exhibits the center-filled X-ray morphology typical of mixed-morphology SNRs: the X-ray spectrum of this SNR features noticeable Si and S lines and can be fit adequately with thermal models, indicating that the X-ray emitting gas is close to ionization equilibrium. No clear X-ray spectral variations are seen across this SNR. In contrast to HB21, the X-ray emission from CTB 1 extends beyond the incomplete radio shell of the SNR. The spectrum of the X-ray emission from CTB 1 features lines associated with Mg, Si, Ca and Ar and is harder than the emission from HB21. This result indicates that either the X-ray emitting gas associated with this SNR has not yet attained thermal equilibrium or this emission has multiple thermal components. We compare X-ray properties of HB21 and CTB 1 with other mixed-morphology SNRs as published in the literature.
The author(s) of this abstract have provided an email address for comments about the abstract: tpannuti@ipac.caltech.edu
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Bulletin of the American Astronomical Society, 36 #3
© 2004. The American Astronomical Soceity.