Dynamical Evolution of Steller Systems with Steller Evolution Included

包含 Steller Evolution 的 Steller 系统的动态演化

基本信息

批准号：
09640310
负责人：
SUGIMOTO Daiichiro
金额：
$ 1.92万
依托单位：
University of the Air
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
1997
资助国家：
日本
起止时间：
1997 至 1998
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-09640310/
关键词：
stellar system self-gravitating many-body system planetary system formation large-scale structure of the universe globular cluster stellar evolution numerical simulation Fokker-Planck approximation シミュレーションフォッカー・プランク近似恒星系力学恒星進化論 /

项目摘要

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.

研究了恒星系统等自引力系统的演化，其中考虑了系统各组成部分与演化的相互作用。主题包括各种各样的现象，例如行星和球状星团的形成、星系核的演化以及宇宙的大尺度结构。在这些不同的现象之间，寻找共同的物理过程及其理解。在众多成就中，以下几点值得注意。对于球状星团，动力学演化的直接多体计算与恒星演化的计算相结合。结果，1）发现球状星团中恒星的蒸发比之前用福克-普朗克近似估计的要慢得多，2）恒星的合并不稳定性被证明发生在年轻致密星团中，如在麦哲伦星云（星系）。球状星团红巨星分支中观测到的元素丰度异常与星团中恒星之间的潮汐相互作用有关。要使本研究取得进一步进展，首先要建立更可靠的模型用于由系统元件组成的重力相互作用的流体动力系统。典型的例子是恒星之间潮汐相互作用的模型。对于星系和星系团来说，澄清并包括恒星形成的过程非常重要，并且可以在避免数值耗散的情况下进行高精度模拟。