Stellar Dynamics: Exact Solution of the Self-Gravitation Equation
Stellar Dynamics: Exact Solution of the Self-Gravitation Equation
复制标题
恒星动力学：自引力方程的精确解
DOI：
10.1093/mnras/123.5.447
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发表时间：
1961
影响因子：
4.8
通讯作者：
D. Lynden
中科院分区：
文献类型：
--
作者：
D. Lynden
本文给出了非弛豫、自引力、轴对称、稳态恒星系统模型的发现方法。解决的主要问题是找到对应于所观察到的密度变化的分布函数。该方法适用于在一个简单的情况下，给一个单参数家庭这样的精确模型。最后，“松弛条件”，没有星星流，但只有旋转，是强加的。然后系统的密度唯一地指定它。因此，我们能够给出一个准确的描述模型旋转扁平球状星团。
A method is given for the discovery of models for unrelaxed, self gravitating, axialiy-symmetrical, steady-state stellar systems. The main problem solved is to find the distribution function corresponding to an observed density variation. The method is applied in a simple case to give a one-parameter family of such exact models. Finally the “relaxation condition”, that there be no star streaming but only rotation, is imposed. The density of the system then specifies it uniquely. We are thus able to give an exact description of models for rotating flattened globular clusters.