超致密天体能在多大程度上模仿黑洞的环形辐射？
How well can ultracompact bodies imitate black hole ringdowns?
摘要：
新兴的引力波天文学仪器对黑洞合并的持续观测，为检验广义相对论性克尔黑洞度规开辟了道路，同时也为探索更多推测性的无视界超紧天体的存在开辟了道路。在本文中，我们量化的差异，这两类对象可能会表现出合并后的振铃信号。通过考虑旋转系统在广义相对论和假设程函极限和三阶Hartle-Thorne慢旋转近似，我们提供了第一个计算的早期振铃频率和阻尼时间作为一个功能的身体的多极结构。使用的例子，重力星，我们表明，主要的振铃信号可能会有百分之几的不同，相对于克尔黑洞，偏差，可以探测到不久的将来先进的LIGO/处女座搜索。
英文摘要：
The ongoing observations of merging black holes by the instruments of the fledging gravitational wave astronomy has opened the way for testing the general relativistic Kerr black hole metric and, at the same time, for probing the existence of more speculative horizonless ultracompact objects. In this paper we quantify the difference that these two classes of objects may exhibit in the post-merger ringdown signal. By considering rotating systems in general relativity and assuming an eikonal limit and a third-order Hartle-Thorne slow rotation approximation, we provide the first calculation of the early ringdown frequency and damping time as a function of the body's multipolar structure. Using the example of a gravastar, we show that the main ringdown signal may differ as much as a few percent with respect to that of a Kerr black hole, a deviation that could be probed by near future Advanced LIGO/Virgo searches.
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