Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...466..866b&link_type=abstract
Astrophysical Journal v.466, p.866
Astronomy and Astrophysics
Astronomy
52
Ism: Supernova Remnants, Hydrodynamics, Ism: Individual Name: Cassiopeia A, Stars: Circumstellar Matter
Scientific paper
We model the Cassiopeia A supernova remnant in the framework of the circumstellar medium (C SM) interaction picture. In this model, the slow red supergiant wind of the supernova (SN) progenitor was swept into a dense shell by a fast stellar wind in the subsequent blue supergiant stage of the progenitor star. The supernova blast wave propagated quickly (≤ 100 yr) through the tenuous wind-blown bubble located within this shell and then slowed down in the dense (nH ˜15 cm-3) CSM shell. The shell was impulsively accelerated during this interaction stage; during the subsequent interaction with SN ejecta, the shell has been further accelerated to ˜2000 km s-1, the currently observed expansion rate. The comparison of our X-ray emission calculations with the ASCA spectrum suggests that about 8 Msun of X- material is present in Cas A. Most of this mass is located in the CSM shell and in the outlying red supergiant wind. The X-ray continuum and the Fe Kα line are dominated by the shell emission, but prominent Kα complexes of Mg, Si, and S must be produced by SN ejecta with strongly enhanced abundances of these elements. Our hydrodynamical models indicate that about 2 Msun of ejecta have been shocked. An explosion of a stellar He core is consistent with these findings.
Blondin John M.
Borkowski Kazimierz
Sarazin Craig L.
Szymkowiak Andrew E.
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