Document Type

Article

Publication Date

8-9-2018

Publication Title

Monthly Notices of the Royal Astronomical Society

Volume

480

Issue

4

First page number:

1

Last page number:

6

Abstract

A circumbinary disc around a pair of merging stellar-mass black holes may be shocked and heated during the recoil of the merged hole, causing a near-simultaneous electromagnetic counterpart to the gravitational wave event. The shocks occur around the recoil radius, where the disc orbital velocity is equal to the recoil velocity. The amount of mass present near this radius at the time of the merger is critical in determining how much radiation is released. We explore the evolution of a circumbinary disc in two limits. First, we consider an accretion disc that feels no torque from the binary. The disc does not survive until the merger unless there is a dead zone, a region of low turbulence. Even with the dead zone, the surface density in this case may be small. Secondly, we consider a disc that feels a strong binary torque that prevents accretion on to the binary. In this case there is significantly more mass in regions of interest at the time of the merger. A dead zone in this disc increases the mass close to the recoil radius. For typical binary-disc parameters we expect accretion to be significantly slowed by the resonant torque from the binary, and for a dead zone to be present. We conclude that provided significant mass orbits the binary after the formation of the black hole binary and that the radiation produced in recoil shocks can escape the flow efficiently, there is likely to be an observable electromagnetic signal from black hole binary mergers.

Keywords

Accretion; Accretion discs; Black hole physics; Gravitational waves; Hydrodynamics; Binaries: General

Disciplines

Astrophysics and Astronomy

File Format

pdf

File Size

300 Kb

Language

English

Rights

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 [owner as specified on the article] Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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