Dynamical Evolution of Steller Systems with Steller Evolution Included

研究了恒星系统等自引力系统的演化，其中考虑了系统每个组成部分与演化的相互作用。课程包括各种各样的现象，如行星和球状星团的形成、星系核的演变以及宇宙的大尺度结构。在这些不同的现象之间，寻求共同的物理过程及其理解。在许多成就中，以下是值得注意的。对于球状星团，将动力学演化的直接多体计算与恒星演化计算结合起来。结果表明：（1）球状星团中恒星的蒸发速度远低于Fokker-Planck近似估计的速度;（2）在麦哲伦星云（星系）中观测到的年轻致密星星团中存在恒星的合并不稳定性。在球状星团红巨星分支观测到的元素丰度异常与星团内恒星之间的潮汐相互作用有关，为进一步开展这一课题的研究，首先应建立更可靠的由该系统元素组成的引力相互作用流体动力学系统模型。典型的例子是恒星之间的潮汐相互作用模型。对于星系和星系团来说，澄清和包括星星形成的过程，并在避免数值耗散的情况下进行高精度的模拟是很重要的。

Evolution of selfgravitating systems such as stellar systems was investigated, where the interactions with evolution of each constituent of the system were taken into account. The subjects included phenomena of wide variety such as formation of planets and globular clusters, evolution of the galactic nuclei, as well as the large-scale structure of the universe. Between these different phenomena, common physical processes and their understandings were sought for. Among many accomplishments, the followings were to be noticed. For the globular clusters the direct many-body calculation of dynamical evolution was combined with calculation of stellar evolution. As a result, 1) evaporation of the stars from the globular cluster is found as much slower than the previous estimate with Fokker-Planck approximation, and 2) the merging instability of the stars was shown to occur in young dense star clusters as observed in the Magellanic Clouds (galaxy). The abundance anomaly of the elements as observed in the red-giant branch of globular cluster is shown as related with tidal interaction between the stars in the cluster.For further progress of this research subject, the first importance should be laid in constructing more reliable models for gravitationally interacting hydrodynamic systems consisting of the elements of the system. Typical example is the model of the tidal interaction between the stars. For the galaxies and the clusters of galaxies it will be important to clarify and include the process of star formation, and to make high accuracy simulations possible where numerical dissipation can be avoided.