The temperature structure in accretion flows onto massive protostars
The temperature structure in accretion flows onto massive protostars
复制标题
吸积过程中的温度结构流向大质量原恒星
DOI：
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发表时间：
1986
期刊：
影响因子：
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通讯作者：
J. Cassinelli
中科院分区：
文献类型：
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作者：
M. Wolfire;J. Cassinelli
研究了恒星形成过程中尘埃和气体入射时的辐射传输问题。讨论了尘埃的性质，并提出了修正的球面辐射传输方程，允许处理相对于壳体内半径的小尺寸恒星的尘埃前向散射。发展了一种计算入射到壳体内缘的恒星辐射场的方法。对Cassinelli和Hartmann(1975)关于扩展恒星大气的温度校正过程进行了修正，以便可以推导出云中颗粒的多温度性质。讨论了密度预先确定的三种示意性模型的温度分布。讨论了颗粒的辐射加速，表明适当的平均不透明度与通常使用的Rosseland平均不透明度相差很大。给出了模型的涌现通量。参考文献56篇。
Radiation transfer problems involved in the infall of dust and gas during star formation are studied. Dust properties are discussed, and modifications of spherical radiative transfer equations are presented that permit forward scattering by dust to be treated for the small size of the star relative to the inner radius of the shell. A procedure for deriving the stellar radiation field incident on the inner edge of the shell is developed. The temperature correction procedure of Cassinelli and Hartmann (1975) for extended stellar atmospheres is modified so that the multitemperature nature of the grains in the cloud may be derived. Temperature distributions for three schematic models in which the density is prespecified are discussed. Radiative acceleration of grains is addressed, showing that the proper mean opacity differs by a large factor from the Rosseland mean opacity that is commonly used. Emergent fluxes for the models are given. 56 references.