Properties of loss cone stars in a cosmological galaxy merger remnant

TL;DR

This study examines the orbital characteristics of stars interacting with a supermassive black hole binary in a galaxy merger remnant, revealing their role in binary hardening and merger timescale.

Contribution

It introduces a hybrid simulation method combining N-body and self-consistent field techniques to analyze loss cone stars in a cosmological galaxy merger remnant.

Findings

Stellar interactions drive SMBH binary hardening effectively.

Loss cone refilling is efficient due to slight triaxiality, avoiding the final parsec problem.

Retrograde interactions are the most energetic, influencing angular momentum changes.

Abstract

Aims: We investigate the orbital and phase space properties of loss cone stars that interact strongly with a hard, high-redshift binary supermassive black hole (SMBH) system formed in a cosmological scenario. Methods: We use a novel hybrid integration approach that combines the direct N-body code $\varphi$-GRAPE with ETICS, a collisionless code that employs the self-consistent field method for force calculation. The hybrid approach shows considerable speed-up over direct summation for particle numbers $> 10^6$, while retaining accuracy of direct N-body for a subset of particles. During the SMBH binary evolution we monitor individual stellar interactions with the binary in order to identify stars that noticeably contribute to the SMBH binary hardening. Results: We successfully identify and analyze in detail the properties of stars that extract energy from the binary. We find that the summed energy changes seen in these stars match very well with the overall binary energy change, demonstrating that stellar interactions are the primary drivers of SMBH binary hardening in triaxial, gas-poor systems. The slight triaxiality of our system results in efficient loss cone refilling, avoiding the final parsec problem. We distinguish three different populations of interactions based on their apocenter. We find a clear prevalence of interactions co-rotating with the binary. Nevertheless, retrograde interactions are the most energetic, contributing only slightly less than the prograde population to the overall energy exchange. The most energetic interactions are also likely to result in a change of sign in the angular momentum of the star. We estimate the merger timescale of the binary to be $\approx 20$ $\mathrm{Myr}$, a value larger by a factor of two than the timescale reported in a previous study.