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Building on a recent paper in which we computed the canonical Hamiltonian ofa spinning test particle in curved spacetime, at linear order in the particle'sspin, we work out an improved effective-one-body (EOB) Hamiltonian for spinningblack-hole binaries. As in previous descriptions, we endow the effectiveparticle not only with a mass m, but also with a spin S*. Thus, the effectiveparticle interacts with the effective Kerr background (having spin S_Kerr)through a geodesic-type interaction and an additional spin-dependentinteraction proportional to S*. When expanded in post-Newtonian (PN) orders,the EOB Hamiltonian reproduces the leading order spin-spin coupling and thespin-orbit coupling through 2.5PN order, for any mass-ratio. Also, itreproduces all spin-orbit couplings in the test-particle limit. Similarly tothe test-particle limit case, when we restrict the EOB dynamics to spinsaligned or antialigned with the orbital angular momentum, for which circularorbits exist, the EOB dynamics has several interesting features, such as theexistence of an innermost stable circular orbit, a photon circular orbit, and amaximum in the orbital frequency during the plunge subsequent to the inspiral.These properties are crucial for reproducing the dynamics andgravitational-wave emission of spinning black-hole binaries, as calculated innumerical relativity simulations.

An improved effective-one-body Hamiltonian for spinning black-hole binaries