银河系中心观测对引力替代理论的限制
Constraints on alternative theories of gravity with observations of the Galactic Center
摘要：
为了评估一个潜在的通常分析测试粒子的轨迹。对于银河系中心的情况，天文学家使用明亮的恒星或光子，因此有两种基本的观测技术来研究引力势，即：（a）在银河系中心附近使用10米凯克双望远镜和4台8米甚大望远镜进行监测，这些望远镜配备有自适应光学设施（此外，最近红外线干涉仪重力开始与甚大望远镜一起工作）;（b）使用毫米波段望远镜，用甚长基线干涉仪技术测量黑洞周围阴影的大小和形状。目前，人们可以使用一个小的相对论修正方法来分析恒星轨道，然而，在未来，由于观测设施的巨大进步，这种近似将不够精确，最近重力小组发现，在S2恒星轨道情况下，必须考虑第一个后牛顿修正。而在VLBI观测中进行最小结构分析时，需要强引力场近似。我们将讨论观察结果及其解释。
英文摘要：
To evaluate a potential usually one analyzes trajectories of test particles. For the Galactic Center case astronomers use bright stars or photons, so there are two basic observational techniques to investigate a gravitational potential, namely, (a) monitoring the orbits of bright stars near the Galactic Center as it is going on with 10m Keck twin and four 8m VLT telescopes equipped with adaptive optics facilities (in addition, recently the IR interferometer GRAVITY started to operate with VLT); (b) measuring the size and shape of shadows around black hole with VLBI-technique using telescopes operating in mm-band. At the moment, one can use a small relativistic correction approach for stellar orbit analysis, however, in the future the approximation will not be precise enough due to enormous progress of observational facilities and recently the GRAVITY team found that the first post-Newtonian correction has to be taken into account for the gravitational redshift in the S2 star orbit case. Meanwhile for smallest structure analysis in VLBI observations one really needs a strong gravitational field approximation. We discuss results of observations and their interpretations.
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