  Accreting black holes (BHs) produce intense radiation and powerful
relativistic jets, which are affected by the BH's spin magnitude and direction.
While thin disks might align with the BH spin axis via the Bardeen-Petterson
effect, this does not apply to jet systems with thick disks. We used fully
three-dimensional general relativistic magnetohydrodynamical simulations to
study accreting BHs with various BH spin vectors and disk thicknesses with
magnetic flux reaching saturation. Our simulations reveal a "magneto-spin
alignment" mechanism that causes magnetized disks and jets to align with the BH
spin near BHs and further away to reorient with the outer disk. This mechanism
has implications for the evolution of BH mass and spin, BH feedback on host
galaxies, and resolved BH images for SgrA* and M87.
