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

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 $16\%-28\%$. 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 $(2,2)$ 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.

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Cited by in corpus (8)

• Magnetically Arrested Circumbinary Accretion Flows
• General Relativistic Magnetohydrodynamic Simulations of Accretion Disks Around Tilted Binary Black Holes of Unequal Mass
• Quasi-periodic oscillation in short gamma-ray bursts from black hole-neutron star mergers
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• Binary black holes in magnetized AGN disks
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• Multimessenger Signatures of Tilted, Self-Gravitating, Black Hole Disks