Magnetic fields regulate black hole (BH) accretion, governing both inflow and outflow dynamics. When a BH accumulates substantial vertical magnetic flux, it enters the magnetically arrested disk (MAD) state, where dynamically important fields power jets and trigger disk eruptions. We investigate MAD evolution when the BH spin and disk angular momentum are misaligned, a likely scenario in many BH systems. Using numerical simulations, we show that jets from rapidly spinning, prograde BHs realign the inner disk via the magneto-spin alignment mechanism for initial tilts up to $\mathcal{T}\lesssim 60°$. Larger tilts lead to intermittent jets that disrupt the disk out to $r\gtrsim 100$ gravitational radii, creating hot cavities and magnetized filaments. These episodic jets form a mini–feedback loop and may explain quasiperiodic X-ray and radio flares observed in low-luminosity active galactic nuclei. We also find that (i) BH spin and disk tilt influence the amount of magnetic flux accumulated at the horizon, and (ii) large-scale, thick, misaligned accretion flows do not exhibit sustained Lense-Thirring (LT) precession. This suggests that slowly accreting BHs ($\dot{M}\ll {10}^{-3}{\dot{M}}_{\text{Edd}}$) are unlikely to show lightcurve quasiperiodic oscillations from LT precession, consistent with observations. Instead, magnetic flux eruptions drive jet wobbling and lateral motion, offering an alternative explanation for phenomena such as the M87 jet’s apparent precession and rapid swings in blazar jet orientation.

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• Classical black holes
• Electromagnetic radiation astronomy
• Fluids & classical fields in curved spacetime
• Accretion disk & black-hole plasma
• Astrophysical jets
• Normal galaxies
• Astrophysical electromagnetic fields
• Astrophysical & cosmological simulations