Adiabatic equatorial inspirals of a spinning body into a Kerr black hole

The detection of gravitational waves from extreme mass ratio inspirals (EMRIs) by the future space-based gravitational-wave detectors demands generation accurate enough waveform templates. Since spin smaller secondary body cannot be neglected for and parameter estimation EMRIs, we study its influence on phase EMRIs with a spinning secondary. We focus generic eccentric equatorial orbits around Kerr black hole. To model object, use Mathisson-Papapetrou-Dixon equations in pole-dipole approximation. Furthermore, linearize orbital variables fluxes respective orbits. obtain these using Teukolsky formalism frequency domain. derive evolution spin-induced corrections to adiabatic an inspiral. Finally, through their numerical integration, find shift between inspiral nonspinning body.