Accretion during the merger of supermassive black holes Export

@article{citeulike:3649154, abstract = {We study the evolution of disk accretion during the merger of supermassive black hole binaries in galactic nuclei. In hierarchical galaxy formation models, the most common binaries are likely to arise from minor galactic mergers, and have unequal mass black holes. Once such a binary becomes embedded in an accretion disk at a separation of the order of 0.1 pc, the merger proceeds in two distinct phases. During the first phase, the loss of orbital angular momentum to the gaseous disk shrinks the binary on a timescale of \~{}10 Myr. The accretion rate onto the primary black hole is not increased, and can be substantially reduced, during this disk-driven migration. At smaller separations, gravitational radiation becomes the dominant angular momentum loss process, and any gas trapped inside the orbit of the secondary is driven inwards by the inspiralling black hole. The implied accretion rate just prior to coalescence exceeds the Eddington limit, so the final merger is likely to occur within a common envelope formed from the disrupted inner disk, and be accompanied by high velocity (\~{}10,000 km/s) outflows.}, archivePrefix = {arXiv}, author = {Armitage, Philip J. and Natarajan, Priyamvada}, citeulike-article-id = {3649154}, citeulike-linkout-0 = {http://arxiv.org/abs/astro-ph/0201318}, citeulike-linkout-1 = {http://arxiv.org/pdf/astro-ph/0201318}, day = {18}, eprint = {astro-ph/0201318}, keywords = {accretion, active, black, disks, galaxies, general, gravitational, hole, nuclei, physics, quasars, waves}, month = {Jan}, posted-at = {2008-11-21 14:48:43}, priority = {0}, title = {Accretion during the merger of supermassive black holes}, url = {http://arxiv.org/abs/astro-ph/0201318}, year = {2002} }

TY - JOUR ID - citeulike:3649154 L3 - citeulike-article-id:3649154 N2 - We study the evolution of disk accretion during the merger of supermassive black hole binaries in galactic nuclei. In hierarchical galaxy formation models, the most common binaries are likely to arise from minor galactic mergers, and have unequal mass black holes. Once such a binary becomes embedded in an accretion disk at a separation of the order of 0.1 pc, the merger proceeds in two distinct phases. During the first phase, the loss of orbital angular momentum to the gaseous disk shrinks the binary on a timescale of ~10 Myr. The accretion rate onto the primary black hole is not increased, and can be substantially reduced, during this disk-driven migration. At smaller separations, gravitational radiation becomes the dominant angular momentum loss process, and any gas trapped inside the orbit of the secondary is driven inwards by the inspiralling black hole. The implied accretion rate just prior to coalescence exceeds the Eddington limit, so the final merger is likely to occur within a common envelope formed from the disrupted inner disk, and be accompanied by high velocity (~10,000 km/s) outflows. TI - Accretion during the merger of supermassive black holes KW - accretion KW - active KW - black KW - disks KW - galaxies KW - general KW - gravitational KW - hole KW - nuclei KW - physics KW - quasars KW - waves AU - Armitage, Philip AU - Natarajan, Priyamvada PY - 2002/Jan/18/ UR - http://arxiv.org/abs/astro-ph/0201318 ER -