论文标题
通过模拟的NGC 6624中心的中间质量黑洞重新访问证据
Revisiting the Evidence for an Intermediate-mass Black Hole in the Center of NGC 6624 with Simulations
论文作者
论文摘要
LMXB 4U 1820-30的加速源自其轨道衍生物$ \ dot p _ {\ rm b} $被认为是中间质量黑洞（IMBH）的证据主要是由于重力波发射，而不是簇电位的加速度。使用GC的标准结构模型，我们模拟了群集中央区域中脉冲星的加速度分布。通过将J1823-3021A的加速度与模拟分布曲线（最大值）拟合，建议将具有质量$ M \ M \ gtrsim 950^{+550} _ { - 350} 〜M _ {\ odot} $的IMBH居住在群集中心。我们进一步表明，J1823-3021A的第二阶段衍生物$ \ ddot P $可能是由于附近恒星的重力扰动所致。
The acceleration of LMXB 4U 1820-30 that derived from its orbital-period derivative $\dot P_{\rm b}$ was supposed to be the evidence for an Intermediate-mass Black Hole (IMBH) in the Galactic globular cluster (GC) NGC 6624. However, we find that the anomalous $\dot P_{\rm b}$ is mainly due to the gravitational wave emission, rather than the acceleration in cluster potential. Using the standard structure models of GCs, we simulate acceleration distributions for pulsars in the central region of the cluster. By fitting the acceleration of J1823-3021A with the simulated distribution profiles (maximum values), it is suggested that an IMBH with mass $M\gtrsim 950^{+550}_{-350}~M_{\odot}$ may reside in the cluster center. We further show that the second period derivative $\ddot P$ of J1823-3021A is probably due to the gravitational perturbation of a nearby star.
