Primordial stellar evolution - The protostar phase
Primordial stellar evolution - The protostar phase
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原始恒星演化——原恒星阶段
DOI：
10.1086/164018
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发表时间：
1986
期刊：
影响因子：
--
通讯作者：
E. Salpeter
中科院分区：
文献类型：
--
作者：
S. Stahler;F. Palla;E. Salpeter
计算了由纯氢和氦气组成的云形成的原恒星的结构和演化。使用0.0044太阳质量/年的吸积率，云的崩溃是数字如下的一个序列的稳态吸积流到流体静力学的核心，从0.01太阳质量的初始质量增长到10.5太阳质量。在其演化的大部分时间里，核心被光学厚的辐射前体所包围。当质量为1个太阳质量时，核心半径达到47个太阳半径。对于质量足够大的核心，内部深处强烈收缩，驱逐出一个“光度波”，当质量为8个太阳质量时到达表面。这导致核心半径大幅增加，表面对流的建立，以及辐射前兆的消失。导出了核半径与质量和吸积率的关系，并给出了一个新的无金属气体Rosseland平均不透明度表。
The structure and evolution of a protostar forming from a cloud composed of pure hydrogen and helium gas are calculated. Using an accretion rate of 0.0044 solar mass/yr, the collapse of the cloud is followed numerically as a sequence of steady state accretion flows onto the hydrostatic core, which grows from an initial mass of 0.01 solar mass to 10.5 solar masses. The core is surrounded by an optically thick radiative precursor for most of its evolution. The core radius reaches 47 solar radii when the mass is 1 solar mass. For sufficiently massive cores, the deep interior contracts strongly, driving out a 'luminosity wave' which reaches the surface when the mass is 8 solar masses. This results in a large increase in core radius, the establishment of surface convection, and the disappearance of the radiative precursor. The dependence of core radius on the mass and accretion rate is analytically derived, and a new table or Rosseland mean opacities for metal-free gas is presented.