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Binary black-hole coalescence is treated semi-analytically by a novelapproach. Our prescription employs the conservative Skeleton Hamiltonian thatdescribes orbiting Brill-Lindquist wormholes (termed punctures in NumericalRelativity) within a waveless truncation to the Einstein field equations [G.Faye, P. Jaranowski and G. Sch\"afer, Phys. Rev. D {\bf 69}, 124029 (2004)]. Weincorporate, in a transparent Hamiltonian way and in Burke-Thorne gaugestructure, the effects of gravitational radiation reaction into the aboveSkeleton dynamics with the help of 3.5PN accurate angular momentum flux forcompact binaries in quasi-circular orbits to obtain a Semi-Analytic PunctureEvolution to model merging black-hole binaries. With the help of the TaylorT4approximant at 3.5PN order, we perform a {\it first-order} comparison betweengravitational wave phase evolutions in Numerical Relativity and our approachfor equal-mass binary black holes. This comparison reveals that a modifiedSkeletonian reactive dynamics that employs flexible parameters will be requiredto prevent the dephasing between our scheme and Numerical Relativity, similarto what is pursued in the Effective One Body approach. A rough estimate for thegravitational waveform associated with the binary black-hole coalescence in ourapproach is also provided.

Binary Black Hole Coalescence in Semi-Analytic Puncture Evolution