Extreme mass ratio inspiral rates: dependence on the massive black hole mass

We study the rate at which stars spiral into a massive black hole (MBH) due to the emission of gravitational waves (GWs), as a function of the mass M-circle of the MBH. In the context of our model, it is shown analytically that the rate approximately depends on the MBH mass as M-circle(-1/4). Numerical simulations confirm this result, and show that for all MBH masses, the event rate is highest for stellar black holes, followed by white dwarfs, and lowest for neutron stars. The Laser Interferometer Space Antenna (LISA) is expected to see hundreds of these extreme mass ratio inspirals per year. Since the event rate derived here formally diverges as M-circle -> 0, the model presented here cannot hold for MBHs of masses that are too low, and we discuss what the limitations of the model are.