arXiv 2108.097092021-08astro-ph.GAgr-qc

用S星测试银河系中心的势能

Testing the Galactic Centre potential with S-stars

Alexander F. Zakharov

备注：: 4 pages, a number of corrections were done in accordance with a version accepted in MNRAS Letters
DOI：: 10.1093/mnrasl/slab111

摘要：

几十年来，两组天文学家使用大型望远镜凯克和VLT观察银河系中心附近明亮恒星的轨迹。根据他们的观测结果，天文学家得出结论，恒星的轨道大致是椭圆形的，轨道的焦点大致与银河系中心的位置重合。在过去的几年里，一个自引力的暗物质核心-晕分布的建议，由Ruffini，Arguelles，Rueda（RAR）和这个模型被积极地用于随后的研究。特别是，最近有人声称，RAR模型提供了一个更好的适合的轨迹的明亮的恒星相比，传统的模型与超大质量黑洞。暗物质的分布与一个致密的核心具有一个恒定的密度，因为它是建议在RAR模型离开椭圆形的恒星轨道像开普勒的两体问题。然而，在这种情况下，椭圆的焦点并不与银河系中心重合，而是与它们的中心重合，而轨道周期并不取决于半长轴。这些性质与亮星轨道的观测数据不一致。

英文摘要：

Two groups of astronomers used the large telescopes Keck and VLT for decades to observe trajectories of bright stars near the Galactic Centre. Based on results of their observations the astronomers concluded that trajectories of the stars are roughly elliptical and foci of the orbits are approximately coincide with the Galactic Centre position. In a last few years a self-gravitating dark matter core--halo distribution was suggested by Ruffini, Arguelles, Rueda (RAR) and this model was actively used in consequent studies. In particular, recently it has been claimed that the RAR-model provides a better fit of trajectories of bright stars in comparison to the conventional model with a supermassive black hole. The dark matter distribution with a dense core having a constant density as it was suggested in the RAR-model leaves trajectories of stars elliptical like in Kepler's two-body problem. However, in this case not the foci of the ellipses coincide with the Galactic Center but their centers while the orbital periods do not depend on semi-major axes. These properties are not consistent with the observational data for trajectories of bright stars.

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