Origin of the S Stars in the Galactic Center
Origin of the S Stars in the Galactic Center
复制标题
DOI：
10.1086/591734
复制
发表时间：
2008-07
期刊：
影响因子：
--
通讯作者：
Ulf Löckmann;H. Baumgardt;P. Kroupa
中科院分区：
文献类型：
--
作者：
Ulf Löckmann;H. Baumgardt;P. Kroupa
在过去的15年里，在我们银河系的中央秒差距内观察到了大约100颗非常年轻的恒星。虽然可以通过吸积盘中的星星形成来理解从超大质量黑洞（SMBH）形成一个或两个恒星盘的年轻恒星的存在，但在SMBH附近观察到的S星的起源仍然是一个主要的谜团。在这里，我们表明，S星是一个自然的结果，动力学相互作用的两个恒星盘在较大的半径。由于岁差和Kozai相互作用，个别恒星在随机方向上达到极高的离心率。在这种偏心轨道上的双星由于靠近SMBH的通道而被破坏，留下一颗S星星在一个更紧密的轨道上。剩下的星星可能是从SMBH附近被喷射出来的，从而同时为银河系晕中观察到的超高速恒星提供了解释。
Over the last 15 years, around a hundred very young stars have been observed in the central parsec of our Galaxy. While the presence of young stars forming one or two stellar disks at ≈0.1 pc from the supermassive black hole (SMBH) can be understood through star formation in accretion disks, the origin of the S stars observed a factor of 10 closer to the SMBH has remained a major puzzle. Here we show the S stars to be a natural consequence of dynamical interaction of two stellar disks at larger radii. Due to precession and Kozai interaction, individual stars achieve extremely high eccentricities at random orientation. Stellar binaries on such eccentric orbits are disrupted due to close passages near the SMBH, leaving behind a single S star on a much tighter orbit. The remaining star may be ejected from the vicinity of the SMBH, thus simultaneously providing an explanation for the observed hypervelocity stars in the Milky Way halo.