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Using N􀀀body-SPH simulations we study the evolution of the separation of a pair of SMBHsembedded in a star forming circumnuclear disk CNDa. This type of disk is expected to be formedin the central kilo parsec of the remnant of gas-rich galaxy mergers. Our simulations indicate thatorbital decay of the SMBHs occurs more quickly when the mean density of the CND is higher,due to increased dynamical friction. However, in simulations where the CND is fragmented in highdensity gaseous clumps clumpy CND, the orbits of the SMBHs are erratically perturbed by thegravitational interaction with these clumps, delaying, in some cases, the orbital decay of the SMBHs.The densities of these gaseous clumps in our simulations and in recent studies of clumpy CNDs aretwo orders of magnitude higher than the observed density of molecular clouds in isolated galaxies orULIRGs, thus, we expect that SMBH orbits are perturbed less in real CNDs than in the simulatedCNDs of this study and other recent studies. We also nd that the migration timescale has a weakdependence on the star formation rate of the CND. Furthermore, the migration timescale of a SMBHpair in a star-forming clumpy CND is at most a factor three longer than the migration timescale ofa pair of SMBHs in a CND modeled with more simple gas physics. Therefore, we estimate that themigration timescale of the SMBHs in a clumpy CND is on the order of 107 yrsNota general

Artículo de publicación ISI

Author: Valle, L. del; - Escala Astorquiza, Andrés; - Maureira Fredes, C.; - Molina, J.; - Cuadra, J.; - Amaro Seoane, P.; -



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