What produces the diffuse X-ray emission from the Orion nebula? I. Simple spherical models

被引：26

作者：

Arthur, S. J. ^{[1
]}

机构：

[1] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 421卷 / 02期

关键词：

hydrodynamics; stars:; winds; outflows; ISM: bubbles; H II regions; H-II-REGIONS; SELF-SIMILAR EVOLUTION; WIND-BLOWN BUBBLES; MASSIVE STARS; INTERSTELLAR BUBBLES; IONIZING-RADIATION; CROSS-SECTIONS; ENERGY-BALANCE; FLOWS; M17;

D O I：

10.1111/j.1365-2966.2011.20388.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The expansion of stellar wind bubbles inside evolving H II regions is studied in spherical symmetry, with stellar wind parameters and ionizing photon rate appropriate to theta(1)OriC, the main exciting source of the Orion nebula. The effects of mass loading due to embedded proplyds and thermal conduction at the edge of the hot, shocked stellar wind bubble on the expansion are investigated. The predicted X-ray luminosities and spectra of these models are calculated and compared to published observations. The models all have excess emission at higher energies compared to the observations. This emission comes from hot gas behind the stellar wind shock and its temperature depends solely on the stellar wind velocity, which for theta(1)OriC is well established. Possible mechanisms for lowering the temperature of this gas are discussed.

引用

页码：1283 / 1297

页数：15

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