We demonstrate that the generic charged rotating regular black hole
solutions of general relativity coupled to non-linear electrodynamics,
obtained by using the alternate Newman-Janis algorithm, introduces only
small (on level 10-2) inconsistency in the behaviour of the
electrodynamics Lagrangian. This approves application of these analytic
and simple solutions as astrophysically relevant, sufficiently precise
approximate solutions describing rotating regular black holes.
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The possibility that two toroidal accretion configurations may be
orbiting around a super-massive Kerr black hole has been addressed. Such
tori may be formed during different stages of the Kerr attractor
accretion history. We consider the relative rotation of the tori and the
corotation or counterrotation of a single torus with respect to the Kerr
attractor. We give classification of the couples of accreting and non-
accreting tori in dependence on the Kerr black hole dimensionless spin.
We demonstrate that only in few cases a double accretion tori system may
be formed under specific conditions.
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We study ultrahigh-energy particle collisions and optical effects in the
extraordinary class of mining braneworld Kerr-Newman (KN) naked
singularity spacetimes, predicting extremely high efficiency of
Keplerian accretion, and compare the results to those related to the
other classes of the KN naked singularity and black hole spacetimes. We
demonstrate that in the mining KN spacetimes the ultrahigh center-of-
mass energy occurs for collisions of particles following the extremely-
low-energy stable circular geodesics of the "mining regime," colliding
with large family of incoming particles, e.g., those infalling from the
marginally stable counter-rotating circular geodesics. This is
qualitatively different situation in comparison to the standard KN naked
singularity or black hole spacetimes where the collisional ultrahigh
center-of-mass energy can be obtained only in the near-extreme
spacetimes. We also show that observers following the stable circular
geodesics of the mining regime can register extremely blue-shifted
radiation incoming from the Universe, and see strongly deformed sky due
to highly relativistic motion along such stable orbits. The strongly
blue-shifted radiation could be thus a significant source of energy for
such orbiting observers.
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We provide a simple derivation of the corrections for Schwarzschild and
Schwarzschild-Tangherlini black hole entropy without knowing the details
of quantum gravity. We will follow the ideas of Bekenstein, Wheeler, and
Jaynes, using summation techniques without calculus approximations, to
directly find logarithmic corrections to the well-known entropy formula
for black holes. Our approach is free from pathological behavior giving
negative entropy for small values of black hole mass M . With the aid of
the "universality" principle, we will argue that this purely classical
approach could open a window for exploring properties of quantum
gravity.
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In our previous work (Paper I) we applied several models of high-
frequency quasi-periodic oscillations (HF QPOs) to estimate the spin of
the central compact object in three Galactic microquasars assuming the
possibility that the central compact body is a super-spinning object (or
a naked singularity) with external spacetime described by Kerr geometry
with a dimensionless spin parameter a ≡ cJ/GM2 > 1. Here
we extend our consideration, and in a consistent way investigate
implications of a set of ten resonance models so far discussed only in
the context of a < 1. The same physical arguments as in Paper I are
applied to these models, I.e. only a small deviation of the spin
estimate from a = 1, a ≳ 1, is assumed for a favoured model. For five of
these models that involve Keplerian and radial epicyclic oscillations we
find the existence of a unique specific QPO excitation radius.
Consequently, there is a simple behaviour of dimensionless frequency M ×
νU(a) represented by a single continuous function having
solely one maximum close to a ≳ 1. Only one of these models is
compatible with the expectation of a ≳ 1. The other five models that
involve the radial and vertical epicyclic oscillations imply the
existence of multiple resonant radii. This signifies a more complicated
behaviour of M × νU(a) that cannot be represented by single
functions. Each of these five models is compatible with the expectation
of a ≳ 1.
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We study scalar and electromagnetic perturbations of a family of
nonsingular nonrotating black hole spacetimes that are solutions in a
large class of conformally invariant theories of gravity. The effective
potential for scalar perturbations depends on the exact form of the
scaling factor. Electromagnetic perturbations do not feel the scaling
factor, and the corresponding quasinormal mode spectrum is the same as
in the Schwarzschild metric. We find that these black hole metrics are
stable under scalar and electromagnetic perturbations. Assuming that the
quasinormal mode spectrum for scalar perturbations is not too different
from that for gravitational perturbations, we can expect that the
calculation of the quasinormal mode spectrum and the observation with
gravitational wave detectors of quasinormal modes from astrophysical
black holes can constrain the scaling factor and test these solutions.
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In Cardoso et al. [6] it was claimed that quasinormal modes which any
stationary, spherically symmetric and asymptotically flat black hole
emits in the eikonal regime are determined by the parameters of the
circular null geodesic: the real and imaginary parts of the quasinormal
mode are multiples of the frequency and instability timescale of the
circular null geodesics respectively. We shall consider asymptotically
flat black hole in the Einstein-Lovelock theory, find analytical
expressions for gravitational quasinormal modes in the eikonal regime
and analyze the null geodesics. Comparison of the both phenomena shows
that the expected link between the null geodesics and quasinormal modes
is violated in the Einstein-Lovelock theory. Nevertheless, the
correspondence exists for a number of other cases and here we formulate
its actual limits.
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In our previous work we applied several models of high-frequency quasi-
periodic oscillations to estimate the spin of the central compact object
in three Galactic microquasars. We also assumed the possibility that the
central compact body is a super-spinning object. Here we extend our
consideration and investigate in a consistent way the implications of
several resonance models so far discussed only in the context of black
holes.
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Conformal gravity can elegantly solve the problem of spacetime
singularities present in Einstein's gravity. For every physical
spacetime, there is an infinite family of conformally equivalent
singularity-free metrics. In the unbroken phase, every non-singular
metric is equivalent and can be used to infer the physical properties of
the spacetime. In the broken phase, a Higgs-like mechanism should select
a certain vacuum, which thus becomes the physical one. However, in the
absence of the complete theoretical framework we do not know how to
select the right vacuum. In this paper, we study the energy conditions
of non-singular black hole spacetimes obtained in conformal gravity
assuming they are solutions of Einstein's gravity with an effective
energy-momentum tensor. We check whether such conditions can be helpful
to select the vacuum of the broken phase.
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This comment is devoted to the recalculation of the Casimir energy of a
massless scalar field in the Kerr black hole surrounded by quintessence
derived in [B. Toshmatov, Z. Stuchlík and B. Ahmedov, Eur. Phys. J. Plus
132, 98 (2017)] and its comparison with the results recently obtained in
[V. B. Bezerra, M. S. Cunha, L. F. F. Freitas and C. R. Muniz, Mod.
Phys. Lett. A 32, 1750005 (2017)] in the spacetime [S. G. Ghosh, Eur.
Phys. J. C 76, 222 (2016)]. We have shown that in the more realistic
spacetime which does not have the failures illustrated here, the Casimir
energy is significantly bigger than that derived in [V. B. Bezerra, M.
S. Cunha, L. F. F. Freitas and C. R. Muniz, Mod. Phys. Lett. A 32,
1750005 (2017)], and the difference becomes crucial especially in the
regions of near horizons of the spacetime.
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