The star S0-2, which is orbiting Sgr A* with a 15 yr period, almost certainly did not form in situ. We propose that it was injected into this close orbit by the tidal disruption of a massive-star binary, whose primary was more massive than S0-2 and at least 60 M☉. From numerical integrations we find that 1%-2% of incoming binaries with closest approach equal to 130 AU leave the secondary in an orbit with eccentricity within 0.01 of that of S0-2. If additional stars are found orbiting Sgr A* with relatively short periods, they could be used to probe the formation of massive stars in the Galactocentric region, even though the massive stars themselves have long since perished.
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机译：绕Sgr A *绕行15年的恒星S0-2几乎可以肯定没有在原地形成。我们建议，它是由一个大质量恒星双星的潮汐破坏注入到这个近轨道的，该恒星双星的质量比S0-2大，且至少60M☉。从数值积分中我们发现，最接近的方法等于130 AU的传入二进制的1％-2％离开轨道的偏心距在S0-2的0.01以内。如果发现额外的恒星绕Sgr A *绕星周期较短，那么即使这些大质量恒星早已灭亡，它们也可以用来探测在恒河中心地区形成大质量恒星。
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