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Luminous active galactic nuclei (AGN) and X-Ray binaries (XRBs) often containgeometrically thin, radiatively cooled accretion discs. According to theory,these are -- in many cases -- initially highly misaligned with the black holeequator. In this work, we present the first general relativisticmagnetohydrodynamic simulations of very thin (h/r~0.015-0.05) accretion discsaround rapidly spinning (a~0.9) black holes and tilted by 45-65 degrees. Weshow that the inner regions of the discs with h/r<0.03 align with the blackhole equator, though out to smaller radii than predicted by analytic work. Theinner aligned and outer misaligned disc regions are separated by a sharp breakin tilt angle accompanied by a sharp drop in density. We find thatframe-dragging by the spinning black hole overpowers the disc viscosity, whichis self-consistently produced by magnetized turbulence, tearing the disc apartand forming a rapidly precessing inner sub-disc surrounded by a slowlyprecessing outer sub-disc. We find that the system produces a pair ofrelativistic jets for all initial tilt values. At small distances the blackhole launched jets precess rapidly together with the inner sub-disc, whereas atlarge distances they partially align with the outer sub-disc and precess moreslowly. If the tearing radius can be modeled accurately in future work,emission model independent measurements of black hole spin based onprecession-driven quasi-periodic oscillations may become possible.

Disc Tearing and Bardeen-Petterson Alignment in GRMHD Simulations of Highly Tilted Thin Accretion Discs