http://arxiv.org/abs/1601.08082
In this paper, we study gravitational-wave (GW) emission from a hypothetical supermassive black-hole (SMBH) binary at the center of M87. The existence of a SMBH other than that usually identified with the central AGN is a possible explanation for the observed displacement ($\sim O(1)~{\rm pc}$) between the AGN and the galactic centroid, and it is reasonable to assume considering the evolution of SMBHs through galaxy mergers. Because the period of the binary and the resulting GWs is much longer than the observational time span, we calculate the variation of the GW amplitude, rather than the amplitude itself. We investigate the dependence on the orbital elements and the second BH mass taking the observational constraints into account, and discuss the detectability of the GWs with a pulsar timing array.
N. Yonemaru, H. Kumamoto, S. Kuroyanagi, et. al.
Mon, 1 Feb 16
40/42
Comments: 5 pages, 6 figures
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