Magnetosonic Waves as a Driver of Observed Temperature Fluctuation Patterns in AGN Accretion Disks

TL;DR

This study uses 3D simulations to show that magnetosonic waves driven by magnetic turbulence can explain observed temperature fluctuations in AGN accretion disks, matching their speed and amplitude.

Contribution

It demonstrates that magnetosonic waves in turbulent magnetic disks account for observed temperature variability, highlighting the importance of magnetic turbulence over mean-field stresses.

Findings

Wave-like temperature perturbations propagate at magnetosonic speeds.

Fluctuation amplitudes of 2-4% match observational data.

Waves are absent in photosphere, likely due to magnetic dominance and non-equilibrium conditions.

Abstract

Recent observations have revealed slow, coherent temperature fluctuations in AGN disks that propagate both inward and outward at velocities of $\sim 0.01 - 0.1c$, a kind of variability that is distinct from reverberation (mediated by the reprocessing of light) between different regions of the disk. We investigate the origin and nature of these fluctuations using global 3D radiation-magnetohydrodynamic simulations of radiation and magnetic pressure-dominated AGN accretion disks. Disks with a significant turbulent Maxwell stress component exhibit wave-like temperature perturbations, most evident close to the midplane, whose propagation speeds exactly match the local fast magnetosonic speed and are consistent with the speeds inferred in observations. These fluctuations have amplitudes of $2 - 4\%$ in gas temperature, which are also consistent with observational constraints. Disks that are dominated by mean-field Maxwell stresses do not exhibit such waves. While waves may be present in the body of the disk, we do not find them to be present in the photosphere. Although this may in part be due to low numerical resolution in the photosphere region, we discuss the physical challenges that must be overcome for the waves to manifest there. In particular, the fact that such waves are observed implies that the disk photospheres must be magnetically dominated, since radiative damping from photon diffusion smooths out radiation pressure fluctuations. Furthermore, the gas and radiation fluctuations must be out of local thermodynamic equilibrium.