ON THE ORIGIN OF THE B-STARS IN THE GALACTIC CENTER
ON THE ORIGIN OF THE B-STARS IN THE GALACTIC CENTER
复制标题
银河系中心 B 星的起源
DOI：
10.1088/0004-637x/784/1/23
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
H. Perets
中科院分区：
文献类型：
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作者：
A. Madigan;O. Pfuhl;Y. Levin;S. Gillessen;R. Genzel;H. Perets
我们提出了一个新的直接可观测的统计量，该统计量使用银河系中心大质量黑洞附近恒星的天空位置(x，y)和自行(vx，vy)来识别具有高轨道偏心率的人群。对于轨道周期较大的恒星来说，这是最有用的，因为很难确定其动力学加速度。我们将这一统计应用于来自银河系中心大质量黑洞的半径为0.“1<；p<；25”(∼0.004-1 PC)的B星的数据集。我们将结果与N体模拟的结果进行比较，以区分它们形成的场景。我们发现，数据支持的情景与特定的K-震级间隔强烈相关，对应于不同的零年龄、主序(MS)质量和寿命。具有14≲MK≲15(15-20 M☉，TM=8-13 Myr)的恒星与盘形成起源很好地匹配，而具有MK⩾15(<；15 M☉，TM>；13 Myr)的恒星如果各向同性分布，形成的群体更偏心，而不是热的，这表明它们是丘陵双星分裂的起源。
We present a new directly observable statistic that uses sky position (x, y) and proper motion (vx, vy) of stars near the massive black hole in the Galactic center to identify populations with high orbital eccentricities. It is most useful for stars with large orbital periods for which dynamical accelerations are difficult to determine. We apply this statistic to a data set of B-stars with a projected radii 0.″1 < p < 25″ (∼0.004–1 pc) from the massive black hole in the Galactic center. We compare the results with those from N-body simulations to distinguish between scenarios for their formation. We find that the scenarios favored by the data correlate strongly with particular K-magnitude intervals, corresponding to different zero-age, main-sequence (MS) masses and lifetimes. Stars with 14 ≲ mK ≲ 15 (15–20 M☉, tMS = 8–13 Myr) match a disk formation origin well, whereas those with mK ⩾ 15 (<15 M☉, tMS > 13 Myr), if isotropically distributed, form a population that is more eccentric than thermal, which suggests a Hills binary-disruption origin.
DOI：
10.1088/0004-637x/708/1/834
发表时间：
2009-08
期刊：
The Astrophysical Journal
影响因子：
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作者：
H. Bartko;Fabrice Martins;S. Trippe;T. Fritz;R. Genzel;T. Ott;F. Eisenhauer;S. Gillessen;
通讯作者：
H. Bartko;Fabrice Martins;S. Trippe;T. Fritz;R. Genzel;T. Ott;F. Eisenhauer;S. Gillessen;