We now significantly expand our model to study heterogeneous agents with differing, unknown disutilities.

The details of how gas flows into the galactic nucleus from large cosmic distances and how the SMBH in turn imparts feedback into the galaxy remain unresolved.

Accretion flows in galactic nuclei involve magnetized plasma, and it has been long known that magnetic fields strongly perturb the energetics (Shvartsman 1971

Testing the accuracy of our method by numerically stimulating hydrodynamic spherical bondi accretion.

Our numerical scheme utilizes the GRMHD code KHARMA[1], a performance-portable C++ implementation based on iharm3D; iharm3D is itself an extension of HARM.

The dominant outward energy transport mechanism is convection driven by magnetic reconnection in the magnetosphere near the BH.

To investigate the mechanism driving the turbulence, we explore the physics of the outward flow of energy.

The authors HC, RN, PN, KS, AR, and KC acknowledge support from the Gordon and Betty Moore Foundation and the John Templeton Foundation

This study examines near-inertial gravity wave propagation in deep Mediterranean Sea, focusing on transitions between stratified and homogeneous layers.

This study examines near-inertial gravity wave propagation in deep Mediterranean Sea, focusing on transitions between stratified and homogeneous layers.