Long-wavelength, free–free spectral energy distributions from porous stellar winds
Long-wavelength, free–free spectral energy distributions from porous stellar winds
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来自多孔恒星风的长波长、自由-自由光谱能量分布
DOI：
10.1093/mnras/stw216
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发表时间：
2016
影响因子：
4.8
通讯作者：
R. Ignace
中科院分区：
文献类型：
--
作者：
R. Ignace
考虑了大团对电离风自由-自由谱能量分布的影响。目的是强调微团簇和大团簇效应之间的区别。如果簇的体积填充因子随半径变化，则微簇可以改变SED斜率和通量水平;但是，修改与簇几何体无关。在多大程度上改变宏观丛生SED斜率和通量水平？在解决这个问题，两种特定类型的大团块几何形状进行了探讨：壳碎片（“煎饼”形）和球形团块。分析和半分析的结果来自限制的情况下，团块从来没有掩盖对方。当团块确实重叠时，使用基于孔隙度形式的数值计算。在恒定膨胀、等温和固定电离风的假设下，碎片模型得到的结果与微团簇结果基本相同。质量损失率的测定不受壳碎片孔隙效应的影响。相比之下，球形团块可以导致长波长通量的减少，但这种减少仅对极端体积填充因子有意义。
The influence of macroclumps for free-free spectral energy distributions (SEDs) of ionized winds is considered. The goal is to emphasize distinctions between microclumping and macroclumping effects. Microclumping can alter SED slopes and flux levels if the volume filling factor of the clumps varies with radius; however, the modifications are independent of the clump geometry. To what extent does macroclumping alter SED slopes and flux levels? In addressing the question, two specific types of macroclump geometries are explored: shell fragments ("pancake"-shaped) and spherical clumps. Analytic and semi-analytic results are derived in the limiting case that clumps never obscure one another. Numerical calculations based on a porosity formalism is used when clumps do overlap. Under the assumptions of a constant expansion, isothermal, and fixed ionization wind, the fragment model leads to results that are essentially identical to the microclumping result. Mass-loss rate determinations are not affected by porosity effects for shell fragments. By contrast, spherical clumps can lead to a reduction in long-wavelength fluxes, but the reductions are only significant for extreme volume filling factors.
通过 X 射线发射线轮廓形状建模对 O-STAR 风中孔隙度和质量损失的约束
DOI：
10.1088/0004-637x/770/1/80
发表时间：
2013
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Leutenegger M.A;Cohen D.H;Sundqvist J.O;Owocki S.P.
通讯作者：
Owocki S.P.
不均匀热星风的质量损失 III 加速、聚集的双组分介质中线辐射传输的有效不透明形式主义，以及理论和诊断的第一个结果
DOI：
10.1051/0004-6361/201423570
发表时间：
2014
期刊：
arXiv: Solar and Stellar Astrophysics
影响因子：
--
作者：
Sundqvist J.O;Puls. J;Owocki S.P.
通讯作者：
Owocki S.P.