Spin Evolution of Stellar-mass Black Holes Embedded in AGN disks: Orbital Eccentricity Produces Retrograde Circumstellar Flows

TL;DR

This study uses hydrodynamic simulations to show that orbital eccentricity in stellar-mass black holes within AGN disks can cause a switch in circum-stellar disk flow direction, affecting black hole spin evolution and binary merger predictions.

Contribution

It reveals that moderate orbital eccentricity can disrupt steady-state tidal interactions, leading to retrograde disk flows and influencing black hole spin orientations in AGN environments.

Findings

Eccentric orbits can preserve retrograde CSD flows.

Transition eccentricity scales with local sound speed.

Implications for black hole spin alignment and merger models.

Abstract

Spin evolution of stellar-mass Black Holes (sBHs) embedded in AGN accretion disks is an important process relevant to production of gravitaional waves from binary Black Hole (BBH) merger events through the AGN channel. Since embedded sBHs are surrounded by circum-stellar disks (CSDs), the rotation of CSD gas flows determine the direction of the angular momentum it accretes. In this Letter, we use global 2D hydrodynamic simulations to show that while a disk-embedded sBH on a circular orbit transforms the initial retrograde Keplerian shear of the background accretion disk into a prograde CSD flow, as in the classical picture of companion-disk interaction theory, moderate orbital eccentricity could disrupt the steady-state tidal perturbation and preserve a retrograde CSD flow around the sBH. This switch of CSD orientation occurs at a transition eccentricity that scales nearly proportional with local sound speed. This bifurcation in the CSD flow and thereafter spin-up direction of SBHs leads to formation of a population of nearly anti-aligned sBHs and should be incorporated in future population models of sBH and BBH evolutions.