arXiv 0912.42092009-12astro-ph.SR

热恒星的质量通量

Mass fluxes for hot stars

L. B. Lucy

备注：: Accepted by A&A; 6 pages, 5 figures; minor changes from v1
DOI：: 10.1051/0004-6361/200913400

摘要：

为了理解晚型O型矮星异常小的质量损失率，利用前面描述过的构造运动反转层的代码，从第一性原理导出了（T_{eff}，g）空间中相关部分的质量通量.从这些质量通量，弱风域内确定一个恒星的质量损失率由辐射驱动的风是小于由于核燃烧。最近由Marcolino等人（2009）分析的五颗弱风星都落在这个区域内或边缘。但是，尽管这些恒星的理论质量通量比Vink等人（2000）的公式低约1.4 dex，但观测到的速率仍然不匹配，这可能反映了我们对低密度超音速外流的理解不足。Bouret et al.（2005）还计算了两颗强风O4星的质量通量。当Bouret等人考虑风聚集时，预测结果与发现的质量损失率急剧降低一致。

英文摘要：

In an attempt to understand the extraordinarily small mass-loss rates of late-type O dwarfs, mass fluxes in the relevant part of (T_{eff}, g)-space are derived from first principles using a previously-described code for constructing moving reversing layers. From these mass fluxes, a weak-wind domain is identified within which a star's rate of mass loss by a radiatively-driven wind is less than that due to nuclear burning. The five weak-wind stars recently analysed by Marcolino et al. (2009) fall within or at the edge of this domain. But although the theoretical mass fluxes for these stars are ~ 1.4 dex lower than those derived with the formula of Vink et al. (2000), the observed rates are still not matched, a failure that may reflect our poor understanding of low-density supersonic outflows. Mass fluxes are also computed for two strong-wind O4 stars analysed by Bouret et al. (2005). The predictions agree with the sharply reduced mass loss rates found when Bouret et al. take wind clumping into account.

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