Clumping in the inner winds of hot, massive stars from hydrodynamical line-driven instability simulations
Clumping in the inner winds of hot, massive stars from hydrodynamical line-driven instability simulations
复制标题
流体动力学线驱动不稳定性模拟中热大质量恒星内部风的聚集
DOI：
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发表时间：
2012
期刊：
影响因子：
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通讯作者：
S. Owocki
中科院分区：
文献类型：
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作者：
J. Sundqvist;S. Owocki
我们研究了由直线驱动的恒星风的强的、内在的线去阴影不稳定(LDI)引起的风结构的开始的恒星边缘暗化和光球扰动的影响。线性摄动分析表明，包括临边暗化在内，降低了DIUS辐射的稳定作用，导致即使在风底也有净不稳定增长率。对这种不稳定性的非线性演化进行的数值辐射流体力学模拟表明，与以前假设恒星均匀明亮而没有基座扰动的模型相比，现在的风结构发展得更接近(r。1：1R？)进入光球层。这与对O型恒星的观测结果吻合得多，O型恒星通常表明在风底附近存在强烈的团块。
We investigate the eects of stellar limb-darkening and photospheric perturbations for the onset of wind structure arising from the strong, intrinsic line-deshadowing instability (LDI) of a line-driven stellar wind. A linear perturbation analysis shows that including limb-darkening reduces the stabilizing eect of the diuse radiation, leading to a net instability growth rate even at the wind base. Numerical radiationhydrodynamics simulations of the non-linear evolution of this instability then show that, in comparison with previous models assuming a uniformly bright star without base perturbations, wind structure now develops much closer (r . 1:1R?) to the photosphere. This is in much better agreement with observations of O-type stars, which typically indicate the presence of strong clumping quite near the wind base.