$N-$body dynamics of Intermediate mass-ratio inspirals in globular clusters

Understand

The intermediate mass-ratio inspiral of a stellar compact remnant into an intermediate mass black hole (IMBH) can produce a gravitational wave (GW) signal that is potentially detectable by current ground-based GW detectors (e.g., Advanced LIGO) as well as by planned space-based interferometers (e.g., eLISA).

• Here, we present results from a direct integration of the post-Newtonian $N$-body equations of motion describing stellar clusters containing an IMBH and a population of stellar-mass black holes (BHs) and solar mass stars.
• We take particular care to simulate the dynamics closest to the IMBH, including post-Newtonian effects up to order $2.5$.
• Our simulations show that the IMBH readily forms a binary with a BH companion.