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We study the orbital decay of a pair of massive black holes (BHs) with masses5 * 10^5 and 10^7 M_sun, using hydrodynamical simulations of circumnucleardisks (CNDs) with the alternating presence of sub-grid physics such asradiative cooling, star formation, supernova feedback, BH accretion andfeedback. In the absence of such processes, the orbit of the secondary BHdecays over timescales of ~10 Myr to the center of the CND, where the primaryBH resides. When strong dissipation operates in CNDs, fragmentation intomassive objects the size of giant molecular clouds and with densities in therange 10^4 - 10^7 amu / cm^3 occurs, causing stochastic torques and hits thatcan eject the secondary BH from the midplane. Outside the plane, thelow-density medium provides only weak drag, and the BH return is governed byinefficient dynamical friction. In rare cases, clump-BH interactions can leadto a faster decay. Feedback processes lead to outflows, but do not changesignificantly the overall density of the CND midplane. However, with aspherically distributed BH feedback a hot bubble is generated behind thesecondary, which almost shuts off dynamical friction, a phenomenon we dub "wakeevacuation", leading to delays in the decay of possibly ~0.3 Gyr. We discussthe non-trivial implications on the discovery space of the eLISA telescope. Ourresults suggest the largest uncertainty in predicting BH merger rates lies inthe potentially wide variety of galaxy host systems, with different degrees ofgas dissipation and heating, yielding decay timescales from ~10 to ~300 Myr.

astrophysical journal/the astrophysical journal

The Pairing of Accreting Massive Black Holes in Multiphase Circumnuclear  Disks: the Interplay between Radiative Cooling, Star Formation, and Feedback  Processes