X-rays from mass-loaded supernova remnants in the large magellanic cloud

被引:27
作者
Arthur, SJ
Henney, WJ
机构
[1] Instituto de Astronomía, UNAM, 04510 México D. F.
关键词
ISM; H II regions; hydrodynamics; bubbles; Magellanic Clouds; supernova remnants; X-rays;
D O I
10.1086/176770
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Observations of H II complexes surrounding OB associations in the Large Magellanic Cloud have revealed X-ray luminosities that cannot be explained by stellar winds alone or by supernova remnants (SNRs) evolving inside stellar-wind bubbles. In neither case would there be enough matter inside the bubbles to produce the observed flux. We propose a model in which a SNR evolves inside an extremely diffuse stellar-wind bubble (formed by the OB association stars) but the density in the SNR is augmented through hydrodynamic ablation of cool, dense clumps by the post-blast wave SNR flow. We present hydrodynamic calculations, including a nonequilibrium treatment of the ionization and cooling, of the evolution of such mass-loaded SNRs. We show that the models naturally explain many of the properties of the observed diffuse X-rays. In particular, we find dose quantitative agreement between one of our models and observed parameters of N51D.
引用
收藏
页码:752 / 763
页数:12
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