How close can we approach the event horizon of the Kerr black hole from the detection of gravitational quasinormal modes?

作者：Nakamura Takashi; Nakano Hiroyuki^*

来源：Progress of Theoretical and Experimental Physics, 2016, 2016(4): 041E01.

DOI：10.1093/ptep/ptw026

Using the Wentzel-Kramers-Brillouin method, we show that the peak location (r(peak)) of the potential, which determines the quasinormal mode frequency of the Kerr black hole, obeys an accurate empirical relation as a function of the specific angular momentum a and the gravitational mass M. If the quasinormal mode with a/M similar to 1 is observed by gravitational wave detectors, we can confirm the black-hole space-time around the event horizon, r(peak) = r(+) + O(root 1-q), where r(+) is the event horizon radius. However, if the quasinormal mode is different from that of general relativity, we are forced to seek the true theory of gravity and/or face the existence of the naked singularity.

• 出版日期2016-4