如何测量Kerr透镜效应中黑洞的质量、自旋和自旋轴方向1：在BH附近有简单源发射的测试情况
How to Measure Black Hole's Mass, Spin and Direction of Spin Axis in Kerr Lens Effect 1: test case with simple source emission near BH
摘要：
通过观测克尔黑洞自旋强引力透镜效应的两个量，提出了一个测量黑洞质量、自旋和自旋轴方向的理论原理。这些可观测的量是由BH附近的光源同时发出的两条光线产生的：到达远处观察者的初级和次级光线，分别是时间上最早的和次级的。探测时间之间的时间延迟和观测到的这些射线的比通量的比率是可观测的量。严格地说，我们的建议是适用于一个单一的突发式（短时间）各向同性排放的来源。通过适当地总结本文的结果，可以将我们的原理推广到复杂排放的情况，这将在以后的工作中处理。
英文摘要：
We propose a theoretical principle to measure the mass, spin and direction of spin axis of Kerr black holes (BHs) through observing 2 quantities of the spinning strong gravitational lens effect of BHs. Those observable quantities are generated by 2 light rays emitted at the same time by a source near the BH: the primary and secondary rays that reach a distant observer, respectively, the earliest and secondary temporally. The time delay between detection times and the ratio of observed specific fluxes of those rays are the observable quantities. Rigorously, our proposal is applicable to a single burst-like (short duration) isotropic emission by the source. An extension of our principle to cases of complicated emissions may be constructed by summing up appropriately the result of this paper, which will be treated in future works.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
