具有不同恒星形成效率和轨道参数的疏散星团动力学演化
Dynamical evolution of the open clusters with different star formation efficiencies and orbital parameters
AI总结：
本文利用直接 N 体模拟研究非位力化疏散星团在不同恒星形成效率与银河轨道下的演化，发现其寿命约为十个轨道周期且主要由恒星形成效率决定，并与 Gaia DR3 观测吻合。
摘要：
疏散星团是动力学系统，其演化受到恒星形成效率和轨道参数等初始条件的关键影响。理解它们的瓦解机制有助于洞察银河系中恒星族群的动力学混合。我们旨在通过考察不同的全局恒星形成效率和轨道特征如何影响星团寿命与结构变化，研究初始非位力化疏散星团的动力学演化和瓦解。基于我们的计算，我们追踪星团演化直至其瓦解时间。我们将疏散星团动力学演化模型与银河系太阳邻域中观测到的疏散星团进行比较。利用高阶直接 N 体模拟，我们对不同银河轨道上的星团演化进行建模，系统改变初始恒星形成效率，以全面探索瓦解机制。模拟表明，疏散星团通常存活约十个轨道周期，星团寿命强烈依赖于全局恒星形成效率，而仅轻微受轨道偏心率影响。我们估计气体驱离时间尺度为 0.9 Myr，初始超新星爆发可有效移除星团中的气体成分。星团的预期寿命（以轨道周期为单位）强烈取决于星团全局恒星形成效率，而仅略微取决于星团轨道偏心率。理论模型表明，Roche-volume 填充参数与近期太阳邻域观测到的 Gaia DR3 星团目录显著一致。通过纳入具有不同恒星形成效率的混合星团样本，我们对银河盘中的疏散星团演化提供了更细致的理解。
英文摘要：
Open star clusters are dynamic systems whose evolution is critically influenced by initial conditions such as star formation efficiency and orbital parameters. Understanding their dissolution mechanisms provides insight into stellar population dynamical mixing in the Milky Way. We aim to investigate the dynamical evolution and dissolution of initially non-virialised open clusters by examining how different global star formation efficiencies and orbital characteristics impact the cluster longevity and structural changes. We followed the evolution of the clusters up to their dissolution time on the basis of our calculations. We compare our open cluster dynamical evolutionary models with the observed open clusters in our Galaxy's solar vicinity. Using high-order direct N-body simulations, we modelled cluster evolution across different Galactic orbits, systematically varying initial star formation efficiencies to comprehensively explore dissolution mechanisms. Our simulations reveal that open clusters typically survive approximately ten orbital periods, with cluster lifetime being strongly dependent on global star formation efficiency and only marginally influenced by orbital eccentricity. We estimate gas expulsion timescales of 0.9 Myr, with initial supernova explosions efficiently removing gaseous components from the cluster. The expected lifetime of the cluster (in units of orbital periods) strongly depends on the cluster global star-formation efficiency and only slightly on the orbital eccentricities of the cluster. The theoretical models demonstrate a remarkable agreement of the Roche-volobe filling parameter with the recent observed Gaia DR3 cluster catalogues in the solar vicinity. By incorporating a mixed sample of clusters with varying star formation efficiencies, we provide a more nuanced understanding of open cluster evolution in the Galactic disc.
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