DR. BADRI KRISHNAN

In this talk the speaker will consider the black hole formed as a result of a binary black hole coalescence. As expected, the final black hole eventually approaches a Kerr solution. We show numerically, in full general relativity and in the highly non-linear merger regime, how the final black hole approaches equilibrium. In particular we show how the infalling radiation wipes out the deviations from Kerr and the rate at which the multipole moments decay to their asymptotic values. We also provide evidence for correlations between the behavior of the horizon and the observed gravitational signal. If confirmed, this would allow us to probe the dynamics of black hole region behind the event horizon by gravitational wave observations.