Response of a circumbinary accretion disc to black hole mass loss

Abstract

We investigate the evolution of the surface density of a circumbinary accretion disc after the mass loss induced by the merger of two supermassive black holes. We first introduce an analytical model, under the assumption of a disc composed of test particles, to derive the surface density evolution of the disc following the mass loss. The model predicts the formation of sharp density peaks in the disc; the model also allows us to compute the typical timescale for the formation of these peaks. To test and validate the model, we run numerical simulations of the process using the Smoothed Particle Hydrodynamics (SPH) code PHANTOM, taking fluid effects into account. We find good agreement in the shape and position of the peaks between the model and the simulations. In a fluid disc, however, the epicyclic oscillations induced by the mass loss can dissipate, and only some of the predicted peaks form in the simulation. To quantify how fast this dissipation proceeds, we introduce an appropriate parameter, and we show that it is effective in explaining the differences between the analytical, collisionless model and a real fluid disc.

10 pages, 11 figures, accepted by MNRAS; added reference in v2. Animations of the simulations are available at http://db.tt/ceqkpmFe

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Cited by in corpus (9)

• Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
• Electromagnetic Counterparts to Massive Black Hole Mergers
• Astrophysics of Super-massive Black Hole Mergers
• Resonances in retrograde circumbinary discs
• Chasing Super-Massive Black Hole merging events with $Athena$ and LISA
• Circumbinary discs around merging stellar-mass black holes
• The Influence of Black Hole Binarity on Tidal Disruption Events
• On the possible electromagnetic manifestations of merging black holes
• A Drop in the Pond: The Effect of Rapid Mass Loss on the Dynamics and Interaction Rate of Collisionless Particles