标题： 质量损失对星团形成的影响。 二。 数值N体积分及进一步应用 显示英文标题

标题： The impact of mass loss on star cluster formation. II. Numerical N-body integration & further applications

摘要： 我们针对由快速质量损失导致的星团生存问题，对我们论文I中的分析进行了N体数值研究。 我们将具有质量分数的解析轨道{\it 对比}和恒星形成效率$\epsilon$与通过N体积分得到的结果进行比较。 我们利用这些结果来论证，如果恒星聚集体要保持结合状态，即使观测表明其恒星形成效率低至30%或更低，它们也必须发展出高结合能的大质量核心。 引入了平均局部能量比$<\sigma^2/|\phi|>$来根据解散临界值$\epsilon$对结合聚集体进行分类。 在较低$\epsilon$值下溶解的聚集体达到最低比例。 我们成功地将这种分类参数应用于Michie-King和Hernquist型分布函数。 Plummer球体是个例外，因为它违反了我们尝试过的这种以及其他分类参数。 差异的原因包括在这种情况下膨胀阶段的能量重新分布不够有效。 显示英文摘要

摘要： We subject to an N-body numerical investigation our analysis of Paper I on the survival of stellar clusters undergoing rapid mass loss. We compare analytical tracks of bound mass-fraction {\it vs} star formation efficiency $\epsilon$ to those obtained with N-body integration. We use these to argue that stellar clusters must develop massive cores of high-binding energy if they are to remain bound despite a star formation efficiency as low as 30% or lower suggested by observations. The average local virial ratio $<\sigma^2/|\phi|>$ is introduced to classify bound clusters as function of their critical $\epsilon$ for dissolution. Clusters dissolving at lower $\epsilon$ achieve the lowest ratio. We applied this classification parameter successfully to Michie-King and Hernquist-type distribution functions. The Plummer sphere is exceptional in that it defies this and other classification parameters we tried. The reasons for the discrepancy include less effective energy redistribution during the expansion phase for this case.