吸积原团中恒星碰撞的Monte Carlo动力学研究
Stellar collisions in accreting protoclusters: a Monte Carlo dynamical study
摘要：
我们探讨吸积原团的行为与Monte Carlo动力学代码，以评估吸积，两体弛豫和恒星碰撞在集群演化中的相对作用。我们证实了Clarke和Bonnell的建议，即恒星碰撞的数量应该按$N^{5/3} \dot M^{2/3}$（独立于其他星团参数，其中N是星团中恒星的数量，$\dot M$是质量吸积的速率）的比例缩放，从而加强了恒星碰撞在人口稠密（大N）的星团中更可能发生的论点。然而，我们发现，克拉克和邦内尔的估计是悲观的，在这个意义上，我们发现，超过99%的恒星碰撞发生在后绝热制度的集群发展到核心崩溃，吸积和两体弛豫的组合驱动。我们讨论了如何列入二进制可能会减少碰撞的数量，通过逆转的核心崩溃，但也注意到，它开辟了另一个碰撞通道，涉及合并的恒星在硬二进制，但未来的Nbody模拟需要为了探索这个问题。
英文摘要：
We explore the behaviour of accreting protoclusters with a Monte Carlo dynamical code in order to evaluate the relative roles of accretion, two body relaxation and stellar collisions in the cluster evolution. We corroborate the suggestion of Clarke & Bonnell that the number of stellar collisions should scale as $N^{5/3} \dot M^{2/3}$ (independent of other cluster parameters, where N is the number of stars in the cluster and $\dot M$ the rate of mass accretion) and thus strengthen the argument that stellar collisions are more likely in populous (large N) clusters. We however find that the estimates of Clarke & Bonnell were pessimistic in the sense that we find that more than 99 % of the stellar collisions occur within the post-adiabatic regime as the cluster evolves towards core collapse, driven by a combination of accretion and two-body relaxation. We discuss how the inclusion of binaries may reduce the number of collisions through the reversal of core collapse but also note that it opens up another collisional channel involving the merger of stars within hard binaries; future Nbody simulations are however required in order to explore this issue.
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