On the Formation of Runaway Stars BN and x in the Orion Nebula Cluster
On the Formation of Runaway Stars BN and x in the Orion Nebula Cluster
复制标题
猎户座星云团中逃逸星 BN 和 x 的形成
DOI：
10.1051/0004-6361/201732472
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发表时间：
2017
期刊：
影响因子：
--
通讯作者：
U. Virginia
中科院分区：
文献类型：
--
作者：
J. Farias;Jonathan C. Tan Dept. of Space;Earth;Environment;C. Astronomy;U. Virginia
我们探讨的方案，从源我在Kleinmann-Low星云的猎户座星云星团（ONC），这是重要的是最近的区域的大质量星星形成的恒星BN和X的动态弹射。这种喷射会导致源I变成一个近距离双星或两颗恒星合并的产物。因此，我们认为二进制二进制遇到的机制，以产生这一事件。通过运行一个大型的$N$体模拟套件，我们发现，当使用参与者通常采用的质量时，几乎不可能匹配观察结果，特别是源I质量为$7\：{\rm{M}}_\odot$。重现事件的唯一方法是如果源I更大，即，{\rm{M}}_\odot$.然而，即使在这种情况下，再现所观察到的系统的可能性也很低。我们讨论了这些结果的影响，了解这个重要的恒星形成区域。
We explore scenarios for the dynamical ejection of stars BN and x from source I in the Kleinmann-Low nebula of the Orion Nebula Cluster (ONC), which is important for being the closest region of massive star formation. This ejection would cause source I to become a close binary or a merger product of two stars. We thus consider binary-binary encounters as the mechanism to produce this event. By running a large suite of $N$-body simulations, we find that it is nearly impossible to match the observations when using the commonly adopted masses for the participants, especially a source I mass of $7\:{\rm{M}}_\odot$. The only way to recreate the event is if source I is more massive, i.e., $\sim20\:{\rm{M}}_\odot$. However, even in this case, the likelihood of reproducing the observed system is low. We discuss the implications of these results for understanding this important star-forming region.
影响因子：
6.5
作者：
K. Menten;M. Reid;J. Forbrich;J. Forbrich;A. Brunthaler
通讯作者：
K. Menten;M. Reid;J. Forbrich;J. Forbrich;A. Brunthaler