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首页> 外文期刊>The Astrophysical journal >THE IMPACT OF UNRESOLVED BINARIES ON SEARCHES FOR WHITE DWARFS IN OPEN CLUSTERS
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THE IMPACT OF UNRESOLVED BINARIES ON SEARCHES FOR WHITE DWARFS IN OPEN CLUSTERS

机译：未解决的二元数对开放集群中白矮星搜索的影响

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Many open clusters have a deficit of observed white dwarfs (WDs) compared with predictions of the number of stars that evolve into WDs. We evaluate the number of WDs produced in open clusters and the number of those WDs that are detectable using photometric selection techniques. This calculation includes the effects of varying the initial mass function (IMF), the maximum progenitor masses of WDs, and the binary fraction. Differences between the calculated number of observable WDs and the actual number of WDs observed in a specific cluster then indicate the true deficit of WDs that must be explained through effects such as dynamical evolution of the cluster or close binary evolution. Observations of WDs in three open clusters, the Hyades, Pleiades, and Praesepe, are compared to the calculated observable populations in those clusters. The results suggest that a large portion of the white dwarf deficit may be explained by the presence of WDs in unresolved binary systems. However, the calculated WD populations still overpredict the number of observable WDs in each cluster. While these calculations cannot determine the cause of this residual white dwarf deficit, potential explanations include a steep high-mass IMF, dynamical evolution of the cluster, or an increased likelihood of equal-mass components in a binary system. Observations of complete WD samples in open clusters covering a range of ages and masses can help to distinguish between these possibilities.
机译：与对演化成WD的恒星数量的预测相比，许多疏散星团缺乏观测到的白矮星（WD）。我们评估在开放簇中产生的WD的数量以及使用光度选择技术可检测到的WD的数量。此计算包括更改初始质量函数（IMF），WD的最大祖细胞质量和二进制分数的影响。计算出的可观察到的WD数量与在特定簇中观测到的WD的实际数量之间的差异则表明了WD的真实缺陷，必须通过诸如簇的动态演化或紧密二元演化之类的效应来解释WD的真实缺陷。将三个开放聚类（Hyades，Pleiades和Praesepe）中的WD观测值与这些聚类中计算出的可观测种群进行比较。结果表明，白矮星赤字的很大一部分可以由未解决的二元系统中WD的存在来解释。但是，计算得出的WD种群仍然高估了每个群集中可观察到的WD的数量。虽然这些计算无法确定造成白矮星残留的原因，但可能的解释包括陡峭的高品质IMF，星团的动态演化或二进制系统中等质量分量的可能性增加。在涵盖一定年龄和质量范围的开放星团中观察完整的WD样本可以帮助区分这些可能性。

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