Stellar Dynamics around a Massive Black Hole II: Resonant Relaxation

TL;DR

This paper develops a first-principles kinetic theory for Resonant Relaxation in stellar systems orbiting massive black holes, incorporating relativistic effects and providing a framework for understanding their long-term dynamical evolution.

Contribution

It extends Gilbert's kinetic theory to include relativistic effects and derives a kinetic equation for Resonant Relaxation in Keplerian stellar systems, unifying scalar and vector RR.

Findings

Derived a kinetic equation describing RR in a 5D reduced space.

Identified the role of wake functions and correlations in secular evolution.

Established a foundation for future applications to axisymmetric discs.

Abstract

We present a first-principles theory of Resonant Relaxation (RR) of a low mass stellar system orbiting a more massive black hole (MBH). We first extend the kinetic theory of Gilbert (1968) to include the Keplerian field of a black hole of mass $M_\bullet$. Specializing to a Keplerian stellar system of mass $M \ll M_\bullet$, we use the orbit-averaging method of Sridhar & Touma (2015; Paper I) to derive a kinetic equation for RR. This describes the collisional evolution of a system of $N \gg 1$ Gaussian Rings in a reduced 5-dim space, under the combined actions of self-gravity, 1 PN and 1.5 PN relativistic effects of the MBH and an arbitrary external potential. In general geometries RR is driven by both apsidal and nodal resonances, so the distinction between scalar-RR and vector-RR disappears. The system passes through a sequence of quasi-steady secular collisionless equilibria, driven by irreversible 2-Ring correlations that accrue through gravitational interactions, both direct and collective. This correlation function is related to a `wake function', which is the linear response of the system to the perturbation of a chosen Ring. The wake function is easier to appreciate, and satisfies a simpler equation, than the correlation function. We discuss general implications for the interplay of secular dynamics and non-equilibrium statistical mechanics in the evolution of Keplerian stellar systems toward secular thermodynamic equilibria, and set the stage for applications to the RR of axisymmetric discs in Paper III.