Extreme mass ratio inspirals and tidal disruption events in nuclear clusters. I. Time dependent rates

TL;DR

This study introduces a computationally efficient, time-dependent model for predicting rates of tidal disruption events, EMRIs, and plunges around massive black holes, emphasizing the importance of time evolution and mass segregation effects.

Contribution

It develops a novel two-population, time-dependent Fokker-Planck approach that captures the dynamic rates of stellar events near black holes, improving upon steady-state models.

Findings

TDE rates decline over time due to mass segregation.

EMRI and plunge rates peak and then decay exponentially.

Time-dependent rates can differ significantly from steady-state estimates.

Abstract

In this paper we develop a computationally efficient, two-population, time-dependent Fokker-Plank approach in the two dimensions of energy and angular momentum to study the rates of tidal disruption events (TDEs), extreme mass ratio inspirals (EMRIs) and direct plunges occurring around massive black holes (MBHs) in galactic nuclei. We test our code by exploring a wide range of the astrophysically relevant parameter space, including MBH masses, galaxy central densities and inner density slopes. We find that mass segregation and, more in general, the time dependency of the distribution function regulate the event rate: TDEs always decline with time, whereas EMRIs and plunges reach a maximum and undergo a subsequent nearly exponential decay. Once suitably normalized, the rates associated to different choices of MBH mass and galaxy density overlap nearly perfectly. Based on this, we provide a simple scaling that allows to reproduce the time-dependent event rates for any MBH mass and underlying galactic nucleus. Although our peak rates are in general agreement with the literature relying on the steady-state (non-time dependent) assumption, those can be sustained on a timescale that strongly depends on the properties of the system. In particular this can be much shorter than a Gyr for relatively light MBHs residing in dense systems. This warns against using steady state models to compute global TDE, EMRI and plunge rates and calls for a more sophisticated, time dependent treatment of the problem.