Black Hole Mergers Induced by Tidal Encounters with a Galactic Centre Black Hole

TL;DR

This paper explores how tidal encounters with massive black holes in galactic centers can induce stellar-mass black hole mergers by increasing eccentricity and reducing merger times, offering a potential explanation for some gravitational wave events.

Contribution

It introduces a new mechanism where tidal encounters can significantly shorten black hole merger times and alter spin orientations, expanding understanding of merger channels near galactic centers.

Findings

Tidal encounters can shorten GW merger times by over 100 to 100,000 times.

Binary orientations can flip, affecting effective spin distributions.

Estimated merger rate from this channel is about 0.6 Gpc^{-3} yr^{-1}.

Abstract

We discuss the properties of stellar mass black hole (BH) mergers induced by tidal encounters with a massive BH at galactic centres or potentially in dense star clusters. The tidal disruption of stellar binaries by a massive BH is known to produce hypervelocity stars. However, such a tidal encounter does not always lead to the break-up of binaries. Since surviving binaries tend to become hard and eccentric, this process can produce BH mergers in principle. For initially circular binaries, we show that the gravitational wave (GW) merger times become shorter by a factor of more than $10^{2}$ ($10^5$) in $10\%$ ($1\%$) of the surviving cases. This reduction is primarily due to the growth in binary's eccentricity at the tidal encounter. We also investigate the effective spins of the survivors, assuming that BH spins are initially aligned with the binary orbital angular momentum. We find that binary orientations can flip in the opposite direction at the tidal encounter. For the survivors with large merger time reduction factors, the effective spin distribution is rather flat. We estimate the merger rate due to the tidal encounter channel to be $\sim 0.6\ \textrm{Gpc}^{-3}\textrm{yr}^{-1}$. This mechanism is unlikely to be the dominant formation channel of BH mergers. However, the current and near-future GW observatories are expected to detect an enormous number of BH mergers. If mergers are found in the vicinity of massive BHs (e.g. the detection of GW lensing echoes or preceding extreme-mass-ratio bursts), this mechanism would provide a possible explanation for their origin.