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arXiv 0802.0046astro-ph
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O型星的X射线发射

X-ray emission from O stars

David H. Cohen

备注：
9 pages; color figures. To appear in IAU Symposium 250, "Massive Stars as Cosmic Engines," Kauai, HI, December 2007; eds. Bresolin, Crowther, & Puls, Cambridge University Press, 2008. The paper posted here has one additional figure (Fig. 6). A b/w version (sans extra figure) is available at http://astro.swarthmore.edu/~cohen/papers/cohen_OstarXrays_bw_kauai2007.pdf
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摘要：

年轻的O型星是强、硬、可变的X射线源，这些特性强烈影响着它们的星周和银河系环境。在大约100万年后，这些恒星稳定下来，成为稳定的软X射线源。我使用高分辨率的X射线光谱和MHD建模表明，年轻的O型恒星，如θ-1猎户座C是很好地解释了磁通道的风冲击的情况。在它们的磁场消散后，较老的O型星通过不稳定的恒星风中的冲击加热产生X射线。在这里，我也使用X射线光谱和数值模拟来证实这一情况。除了阐明O星X射线发射的性质和原因外，O超巨星的高分辨率X射线光谱的建模提供了强有力的证据，表明这些O星的质量损失率被高估了。

英文摘要：

Young O stars are strong, hard, and variable X-ray sources, properties which strongly affect their circumstellar and galactic environments. After ~1 Myr, these stars settle down to become steady sources of soft X-rays. I use high-resolution X-ray spectroscopy and MHD modeling to show that young O stars like theta-1 Ori C are well explained by the magnetically channeled wind shock scenario. After their magnetic fields dissipate, older O stars produce X-rays via shock heating in their unstable stellar winds. Here too I use X-ray spectroscopy and numerical modeling to confirm this scenario. In addition to elucidating the nature and cause of the O star X-ray emission, modeling of the high-resolution X-ray spectra of O supergiants provides strong evidence that mass-loss rates of these O stars have been overestimated.

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