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Self-consistent modelling of star cluster evolution: Initial conditions and the origin of the stellar population II halo of the Milky Way

星团演化的自洽模型：银河系星族II晕的初始条件和起源

基本信息

批准号：
234732163
负责人：
Professor Dr. Pavel Kroupa
金额：
--
依托单位：
Helmholtz-Institut für Strahlen- und Kernphysik
依托单位国家：
德国
项目类别：
Research Grants
财政年份：
2013
资助国家：
德国
起止时间：
2012-12-31 至 2016-12-31
项目状态：
已结题

来源：
https://gepris.dfg.de/gepris/projekt/234732163?language=en
关键词：
Self consistent modelling star cluster

项目摘要

Only recently it became appreciated that information from the earliest phase of globular cluster (GC) evolution, the removal of the residual-gas from which the stars of a GC formed, may still be contained in present-day observational data. This provides a means to back-trace GCs to their probable initial states using self-consistent \Nbody computations. It has furthermore been suggested that the stellar population II halo of the Milky originates from dissolving star clusters and the fraction of Galactic halo stars that have formed in star clusters may be quantified. Since the oldest GCs in our Galaxy have witnessed the formation of the Milky Way (MW) and since gas-expulsion from GCs is influenced by the evolving tidal-field of the MW, the conditions GCs were exposed to at birth allow a reconstruction of the MW's formation history.We therefore aim to perform for the first-time a high-precision \Nbody study to investigate star cluster evolution self-consistently, including residual-gas expulsion, a changing tidal-field environment and classical two-body relaxation driven evolution. The results will disentangle effects driven by these physical processes and the range of allowed initial conditions, given the observational data, will be investigated. This will provide insights into the early star cluster formation processes and will constrain the detailed events of the formation of the Galaxy.

直到最近，人们才意识到，球状星团(GC)演化的最早阶段，即清除形成球状星团恒星的残余气体的信息，可能仍然包含在今天的观测数据中。这提供了一种使用自洽的身体计算回溯GC到其可能的初始状态的方法。此外，有人提出，银河系的星族II晕起源于溶解的星团，形成星团的银河晕星的比例可能是量化的。由于银河系中最古老的星团见证了银河系(MW)的形成，而从GC中排出的气体又受到MW不断演变的潮汐磁场的影响，因此，GC在出生时所暴露的条件允许重建MW的形成历史。因此，我们的目标是首次进行一项高精度的身体研究，以自洽地研究星团演化，包括残余气体排放、不断变化的潮汐场环境和经典的两体弛豫驱动的演化。结果将解开由这些物理过程驱动的影响，并将调查在给定观测数据的情况下允许的初始条件范围。这将提供对早期星团形成过程的洞察，并将限制银河系形成的详细事件。