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THE PUZZLING DYNAMICAL STATUS OF THE CORE OF THE GLOBULAR CLUSTER NGC 6752

机译:球状团簇NGC 6752核心的动态动力学状态

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We have used high-resolution Hubble Space Telescope Wide Field Planetary Camera 2 and ground-based wide-field images to determine the center of gravity and construct an extended radial density and brightness profile of the cluster NGC 6752 including, for the first time, detailed star counts in the very inner region. The barycenter of the nine innermost X-ray sources detected by Chandra is located only 1″.9 off the new center of gravity. Both the density and the brightness profile of the central region are best fitted by a double King model, suggesting that NGC 6752 is experiencing a post-core-collapse bounce. Taking advantage of our new optical data, we discuss the puzzling nature of the accelerations displayed by the innermost millisecond pulsars detected in this cluster. We discuss two possible origins to the accelerations: (1) the overall cluster gravitational potential, which would require a central projected mass-to-light ratio of the order of 6-7 and the existence of a few thousand solar masses of low-luminosity matter within the inner 0.08 pc of NGC 6752, and (2) the existence of a local perturber(s) of the pulsar dynamics, such as a recently proposed binary black hole of intermediate (100-200 solar mass) mass.
机译:我们使用高分辨率哈勃太空望远镜广角行星相机2和地面广角图像来确定重心,并构造了NGC 6752星团的扩展径向密度和亮度分布图,其中包括首次恒星位于非常内部的区域。钱德拉(Chandra)检测到的九个最里面的X射线源的重心位于距新重心仅1''。9的位置。中心区域的密度和亮度分布都可以通过双King模型得到最佳拟合,这表明NGC 6752正在经历核后崩溃反弹。利用我们的新光学数据,我们讨论了在该星团中检测到的最里面的毫秒脉冲星所显示的加速度的令人困惑的性质。我们讨论了加速的两个可能的起源:(1)整体星团的引力,这将需要一个中心投影的质量与光之比约为6-7,并且存在数千个低发光度的太阳质量。 NGC 6752的内部0.08 pc内的物质,以及(2)脉冲星动力学的局部扰动的存在,例如最近提出的中等质量(100-200太阳质量)的二元黑洞。

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