Thin accretion disk around a rotating Kerr-like black hole in Einstein-bumblebee gravity model

TL;DR

This paper investigates the properties of thin accretion disks around a Kerr-like black hole in Einstein-bumblebee gravity, exploring potential observational signatures of Lorentz symmetry breaking.

Contribution

It derives the energy flux, emission spectrum, and efficiency of accretion disks in this modified gravity model, comparing them to the standard Kerr black hole case.

Findings

Differences in energy flux compared to Kerr black holes.

Altered emission spectra due to Lorentz symmetry breaking.

Potential observational tests for Einstein-bumblebee gravity.

Abstract

We study the accretion process in the thin disk around a rotating Kerr-like black hole in Einstein-bumblebee gravity model where Lorentz symmetry is spontaneously broken once a vector field acquires a vacuum expectation value. In the present paper we obtain the energy flux, the emission spectrum and accretion efficiency from the accretion disks around the rotating Kerr-like black hole, and we compare them to the general Kerr case. These significant features in the mass accretion process may provide a possibility to test whether the Lorentz symmetry is spontaneously broken or not in the Einstein-bumblebee gravity model by future astronomical observations.