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51AB14C2-6BB5-4BBC-A246-842E1A0DB676

# Self-gravitating disks around rapidly spinning, tilted black holes: General relativistic simulations

Antonios Tsokaros, Milton Ruiz, Stuart L. Shapiro, Vasileios Paschalidis

Submitted on 9 September 2022

## Abstract

We perform general relativistic simulations of self-gravitating black hole-disks in which the spin of the black hole is significantly tilted (${45}^{\circ }$ and ${90}^{\circ }$) with respect to the angular momentum of the disk and the disk-to-black hole mass ratio is $16\mathrm{%}-28\mathrm{%}$. The black holes are rapidly spinning with dimensionless spins up to $\sim 0.97$. These are the first self-consistent hydrodynamic simulations of such systems, which can be prime sources for multimessenger astronomy. In particular tilted black hole-disk systems lead to: i) black hole precession; ii) disk precession and warping around the black hole; iii) earlier saturation of the Papaloizou-Pringle instability compared to aligned/antialigned systems, although with a shorter mode growth timescale; iv) acquisition of a small black-hole kick velocity; v) significant gravitational wave emission via various modes beyond, but as strong as, the typical $\left(2,2\right)$ mode; and vi) the possibility of a broad alignment of the angular momentum of the disk with the black hole spin. This alignment is not related to the Bardeen-Petterson effect and resembles a solid body rotation. Our simulations suggest that any electromagnetic luminosity from our models may power relativistic jets, such as those characterizing short gamma-ray bursts. Depending on the black hole-disk system scale the gravitational waves may be detected by LIGO/Virgo, LISA and/or other laser interferometers.

## Preprint

Subjects: Astrophysics - High Energy Astrophysical Phenomena; General Relativity and Quantum Cosmology