3 research outputs found
Fluctuations in a Ho\v{r}ava-Lifshitz Bouncing Cosmology
Ho\v{r}ava-Lifshitz gravity is a potentially UV complete theory with
important implications for the very early universe. In particular, in the
presence of spatial curvature it is possible to obtain a non-singular bouncing
cosmology. The bounce is realized as a consequence of higher order spatial
curvature terms in the gravitational action. Here, we extend the study of
linear cosmological perturbations in Ho\v{r}ava-Lifshitz gravity coupled to
matter in the case when spatial curvature is present. As in the case without
spatial curvature, we find that there is no extra dynamical degree of freedom
for scalar metric perturbations. We study the evolution of fluctuations through
the bounce and show that the solutions remain non-singular throughout. If we
start with quantum vacuum fluctuations on sub-Hubble scales in the contracting
phase, and if the contracting phase is dominated by pressure-less matter, then
for and in the infrared limit the perturbations at late times are
scale invariant. Thus, Ho\v{r}ava-Lifshitz gravity can provide a realization of
the ``matter bounce'' scenario of structure formation.Comment: 19 page
Thin accretion disk signatures of slowly rotating black holes in Ho\v{r}ava gravity
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.Comment: 12 pages, 15 figures. V2: 13 pages, clarifications and discussion
added; version accepted for publication in Classical and Quantum Gravit