质量损失率确定的聚团近似法的有效性
Validity of clumping approximations for mass-loss rates determination
摘要：
热恒星的恒星风中的聚团现象是辐射流体动力学方程解中出现的辐射声学不稳定性的一个可能结果。然而，在恒星大气模拟和辐射转移计算中，通常通过一个称为聚团因子的全局自由参数，以高度近似的方式将聚团包括在内。许多研究人员使用不同的聚集因子值成功地更好地拟合了观测到的光谱，并校正了经验质量损失率。这通常导致一个结论，即恒星风是聚集的。为了理解结块如何影响质量损失率的理论预测，必须考虑不同的结块特性。如果结块已经出现在临界点以下，则质量损失率发生变化。
英文摘要：
Clumping in stellar winds of hot stars is a possible consequence of radiative-acoustic instability appearing in solutions of radiative-hydrodynamical equations. However, clumping is usually included to stellar atmosphere modeling and radiative transfer calculations in a highly approximate way via a global free parameter called the clumping factor. Using different values of clumping factors many researchers succeeded to fit the observed spectra better and to correct empirical mass loss rates. This usually leads to a conclusion that the stellar wind is clumped. To understand how clumping may influence theoretical predictions of mass-loss rates, different clumping properties have to be taken into account. If clumping appears already below the critical point, the mass-loss rates is changed.
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