2026/04/30 by Anonymous, Milton Ruiz, Antonios Tsokaros +1
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Pulsars and Gravitational Waves Research #astro-ph.HE #gr-qc
paper · pdf · doi:10.1103/7zd8-yygd
published as Phys. Rev. Lett. 137, 051402 (2026) · 9 pages, 11 figures
openalex publication_date 2026/06/29 · openalex created_date 2026/06/30 · arxiv created 2026/07/28 · arxiv updated 2026/07/30 · openalex updated_date 2026/07/30
We perform fully relativistic GRMHD simulations of magnetized, self-gravitating black hole-disk (BHD) systems in which the black hole spin is misaligned with the disk angular momentum. Massive disks (disk to BH mass ratios of 16-28%) around rapidly rotating black holes (χ\lesssim 0.97) develop a nonaxisymmetric instability for tilt angles from 0^∘ to 180^∘. Magnetic stresses damp, but do not completely suppress, the nonaxisymmetric instability, and corresponding gravitational wave (GW) emission, in aligned systems, while they enhance it in antialigned BHDs: MRI-driven turbulence enhances angular momentum transport and accelerates nonlinear instability evolution in misaligned configurations. All models launch magnetically driven jets consistent with the Blandford-Znajek (BZ) mechanism, with collimation depending on spin orientation. The GWs reflect strong nonaxisymmetric structure from a persistent m=1 mode. The coupling between fast MRI and the slower nonaxisymmetric instability growth governs the outcome, with tilt controlling how MRI modifies the global mode. These simulations provide the first self-consistent GRMHD treatment of tilted, self-gravitating BHD systems and support their role as multimessenger sources.