# Galaxy Rotation and Supermassive Black Hole Binary Evolution

## TL;DR

This paper investigates how galaxy rotation influences supermassive black hole binary evolution using N-body simulations, revealing that orbital plane orientation and eccentricity significantly affect inspiral times, which is crucial for gravitational wave detection.

## Contribution

It provides the first systematic analysis of galaxy rotation effects on SMBH binary evolution with realistic orbital configurations using direct N-body simulations.

## Key findings

- Orbital plane orientation and eccentricity can alter inspiral time by an order of magnitude.
- Galaxy rotation significantly impacts SMBH binary coalescence times.
- Results are important for predicting gravitational wave signals for LISA.

## Abstract

Supermassive black hole (SMBH) binaries residing at the core of merging galaxies are recently found to be strongly affected by the rotation of their host galaxies. The highly eccentric orbits that form when the host is counterrotating emit strong bursts of gravitational waves that propel rapid SMBH binary coalescence. Most prior work, however, focused on planar orbits and a uniform rotation profile, an unlikely interaction configuration. However, the coupling between rotation and SMBH binary evolution appears to be such a strong dynamical process that it warrants further investigation. This study uses direct N-body simulations to isolate the effect of galaxy rotation in more realistic interactions. In particular, we systematically vary the SMBH orbital plane with respect to the galaxy rotation axis, the radial extent of the rotating component, and the initial eccentricity of the SMBH binary orbit. We find that the initial orbital plane orientation and eccentricity alone can change the inspiral time by an order of magnitude. Because SMBH binary inspiral and merger is such a loud gravitational wave source, these studies are critical for the future gravitational wave detector, LISA, an ESA/NASA mission currently set to launch by 2034.