HFQPOs and discoseismic mode excitation in eccentric, relativistic discs. I. Hydrodynamic simulations

TL;DR

This study uses 3D hydrodynamic simulations to demonstrate that eccentric relativistic accretion discs can excite trapped inertial waves, offering insights into the origin of high-frequency quasi-periodic oscillations in black-hole X-ray binaries.

Contribution

First demonstration of excitation of trapped inertial waves by eccentricity in relativistic discs through hydrodynamic simulations, highlighting a potential mechanism for HFQPOs.

Findings

Eccentricity >0.005 near ISCO excites inertial waves.

Excitation of inertial waves is robust across simulation conditions.

Simulations provide proof of concept for wave excitation mechanism.

Abstract

High-frequency quasi-periodic oscillations (HFQPOs) observed in the emission of black-hole X-ray binary systems promise insight into strongly curved spacetime. `Discoseismic' oscillations with frequencies set by the intrinsic properties of the central black hole, in particular `trapped inertial waves' (r-modes), offer an attractive explanation for HFQPOs. To produce an observable signature, however, such oscillations must be excited to sufficiently large amplitudes. Turbulence driven by the magnetorotational instability (MRI) fails to provide the necessary amplification, but r-modes may still be excited via interaction with accretion disc warps or eccentricities. We present 3D global hydrodynamic simulations of relativistic accretion discs, which demonstrate for the first time the excitation of trapped inertial waves by an imposed eccentricity in the flow. While the r-modes' saturated state depends on the vertical boundary conditions used in our unstratified, cylindrical framework, their excitation is unambiguous in all runs with eccentricity >0.005 near the ISCO. These simulations provide a proof of concept, demonstrating the robustness of trapped inertial wave excitation in a non-magnetized context. In a companion paper, we explore the competition between this excitation, and damping by magnetohydrodynamic turbulence.