# Filling the disk hollow following binary black hole merger: The transient accretion afterglow

## TL;DR

This paper models the transient electromagnetic afterglow emitted as a circumbinary disk fills the hollow left by a merging binary black hole, providing insights into observable signatures of such events.

## Contribution

It introduces a simple, time-dependent Newtonian model to simulate the disk's evolution and electromagnetic emission during the post-merger accretion phase.

## Key findings

- Electromagnetic flux increases as the hollow fills.
- Spectrum hardens during the accretion process.
- Potential for super-Eddington accretion during the phase.

## Abstract

Tidal torques from a binary black hole (BHBH) empty out the central regions in any circumbinary gaseous accretion disk. The balance between tidal torques and viscosity maintain the inner edge of the disk at a radius r ~ 1.5a -- 2a, where a is the binary semimajor axis. Eventually, the inspiraling binary decouples from disk and merges, leaving behind a central hollow ("donut hole") in the disk orbiting the remnant black hole. We present a simple, time-dependent, Newtonian calculation that follows the secular (viscous) evolution of the disk as it fills up the hollow down to the black hole innermost stable circular orbit and then relaxes to stationary equilibrium. We use our model to calculate the electromagnetic radiation ("afterglow") spectrum emitted during this transient accretion epoch. Observing the temporal increase in the total electromagnetic flux and the hardening of the spectrum as the donut hole fills may help confirm a BHBH merger detected by a gravitational wave interferometer. We show how the very existence of the initial hollow can lead to super-Eddington accretion during this secular phase if the rate is not very far below Eddington prior to decoupling. Our model, though highly idealized, may be useful in establishing some of the key parameters, thermal emission features and scalings that characterize this transient. It can serve as a guide in the design and calibration of future radiation-magnetohydrodynamic simulations in general relativity.