演講資訊

摘要：

We investigate the influence of magnetic field inclination on accretion dynamics around spinning black holes using axisymmetric general relativistic magnetohydrodynamic (GRMHD) simulations. The study employs a Fishbone-Moncrief torus orbiting a Kerr black hole with spin parameter \(a = 0.9375\), threaded by large-scale magnetic fields inclined at \(30^\circ\), \(45^\circ\), and \(60^\circ\) relative to the spin axis. We explore how magnetic obliquity modifies the field geometry, flow morphology, and angular momentum transport across different initial plasma beta values (\(\beta = 0.007, 0.005, 0.001\)).

Increasing magnetic inclination produces pronounced tilting and deformation of the inner disk, asymmetric outflows, and enhanced temporal variability in accretion rates. The magnetic topology evolves dynamically, with intense reconnection and complex current sheet structures forming near the event horizon -- particularly at lower beta values where magnetic pressure dominates.

Our findings demonstrate that magnetic obliquity critically shapes the structure and variability of relativistic accretion flows, with potential implications for jet orientation and observed variability timescales in active galactic nuclei and other black hole systems.