Thin accretion disk signatures of slowly rotating black holes in Hořava gravity

Details Thin accretion disk signatures of slowly rotating black holes in Hořava gravity Thin accretion disk signatures of slowly rotating black holes in Hořava gravity

2010-09-10

arxiv.org/abs/1009.1958v2

Class.Quant.Grav.28:165001,2011

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

12 pages, 15 figures. V2: 13 pages, clarifications and discussion added; version accepted for publication in Classical and Qua

Scientific paper

10.1088/0264-9381/28/16/165001

In the present work, we consider the possibility of observationally testing Ho\v{r}ava gravity by using the accretion disk properties around slowly rotating black holes of the Kehagias-Sfetsos solution in asymptotically flat spacetimes. The energy flux, temperature distribution, the emission spectrum as well as the energy conversion efficiency are obtained, and compared to the standard slowly rotating general relativistic Kerr solution. Comparing the mass accretion in a slowly rotating Kehagias-Sfetsos geometry in Ho\v{r}ava gravity with the one of a slowly rotating Kerr black hole, we verify that the intensity of the flux emerging from the disk surface is greater for the slowly rotating Kehagias-Sfetsos solution than for rotating black holes with the same geometrical mass and accretion rate. We also present the conversion efficiency of the accreting mass into radiation, and show that the rotating Kehagias-Sfetsos solution provides a much more efficient engine for the transformation of the accreting mass into radiation than the Kerr black holes. Thus, distinct signatures appear in the electromagnetic spectrum, leading to the possibility of directly testing Ho\v{r}ava gravity models by using astrophysical observations of the emission spectra from accretion disks.

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