IX Black Hole Workshop

Guimarães 19-20 December 2016

Gravitational waves from a stellar-mass compact object orbiting a supermassive black hole are one of main targets for future space detectors. These binary systems can be described by the black hole perturbation approach, which uses the mass ratio of the binary as an expansion parameter. At the first order in the mass ratio, orbits of the compact object deviate from Kerr geodesics due to the emission of gravitational waves. The spin of the compact object might also be important to investigate orbits of the compact object at the first order in the mass ratio. In this work, we derive the post-Newtonian formula of the gravitational energy flux from a spinning particle in a circular orbit on the equatorial plane of a Kerr black hole using the black hole perturbation approach. The equation of the motion of the particle is solved to the first order in the particle's spin using pole-dipole approximation. We will estimate how new terms in the energy flux affect the orbital evolution of the particle.