{ "id": "1801.05780", "version": "v1", "published": "2018-01-17T18:10:03.000Z", "updated": "2018-01-17T18:10:03.000Z", "title": "A New Type of Extreme-mass-ratio Inspirals Produced by Tidal Capture of Binary Black Holes", "authors": [ "Xian Chen", "Wen-Biao Han" ], "comment": "5 pages, 2 figures", "categories": [ "astro-ph.HE", "gr-qc" ], "abstract": "Extreme-mass-ratio inspiral (EMRI) is an important gravitational-wave (GW) source and it normally consists of one stellar-mass black hole (BH) whirling closely around a supermassive black hole (SMBH). In this Letter, we demonstrate that the small body, in fact, could be a BH binary (BHB). Our work is motived by previous numerical scatting experiments which show that SMBHs can tidally capture BHBs to bound orbits. Here we investigate the subsequent long-term evolution. We find that only those BHBs with a semi-major axis of $a\\lesssim5\\times10^{-3}$ AU can be captured to tightly-bound orbits such that they will successfully inspiral towards the central SMBHs without being scattered away by stellar relaxation processes. We estimate that these binary-EMRIs (b-EMRIs) could constitute at most a few percent of the EMRI population. Moreover, we show that when the eccentricity of a b-EMRI drops to about $0.85$, the two stellar BHs will quickly merge due to the tidal perturbation by the SMBH. The high-frequency ($\\sim10^2$ Hz) GWs generated during the coalescence coincide with the low-frequency ($\\sim10^{-3}$ Hz) waves from the b-EMRI, making this system an ideal target for future multi-band GW observations.", "revisions": [ { "version": "v1", "updated": "2018-01-17T18:10:03.000Z" } ], "analyses": { "keywords": [ "binary black holes", "extreme-mass-ratio inspiral", "tidal capture", "subsequent long-term evolution", "stellar-mass black hole" ], "note": { "typesetting": "TeX", "pages": 5, "language": "en", "license": "arXiv", "status": "editable" } } }