64 research outputs found
Massive scalar field quasi-normal modes of higher dimensional black holes
We study quasinormal spectrum of massive scalar field in the -dimensional
black hole background. We found the qualitatively different dependence on the
field mass of the fundamental modes for . The behaviour of higher modes
is qualitatively the same for all . Thus for some particular values of mass
(of the field and of the black hole) the spectrum has two dominating
oscillations with a very long lifetime. Also we show that the asymptotically
high overtones do not depend on the field mass. In addition, we present the
generalisation of the Nollert improvement of the continued fraction technique
for the numerical calculation of quasi-normal frequencies of -dimensional
black holes.Comment: 8 pages, 4 figures, misprints corrected, version to appear in Phys.
Rev.
Quasi-Normal Modes of Brane-Localised Standard Model Fields II: Kerr Black Holes
This paper presents a comprehensive study of the fundamental quasinormal
modes of all Standard Model fields propagating on a brane embedded in a
higher-dimensional rotating black hole spacetime. The equations of motion for
fields with spin and 1 propagating in the induced-on-the-brane
background are solved numerically, and the dependence of their QN spectra on
the black hole angular momentum and dimensionality of spacetime is
investigated. It is found that the brane-localised field perturbations are
longer-lived when the higher-dimensional black hole rotates faster, while an
increase in the number of transverse-to-the-brane dimensions reduces their
lifetime. Finally, the quality factor , that determines the best oscillator
among the different field perturbations, is investigated and found to depend on
properties of both the particular field studied (spin, multipole numbers) and
the gravitational background (dimensionality, black hole angular momentum
number).Comment: 12 pages, 8 figures, typos corrected, version to appear in Phys. Rev.
Gravitational instability of simply rotating AdS black holes in higher dimensions
We study the stability of AdS black hole holes rotating in a single two plane
for tensor-type gravitational perturbations in space-time dimensions.
First, by an analytic method, we show that there exists no unstable mode when
the magnitude of the angular momentum is smaller than where
is the horizon radius, and is the AdS curvature radius. Then, by numerical
calculations of quasinormal modes, using the separability of the relevant
perturbation equations, we show that an instability occurs for rapidly rotating
black holes with , although the growth rate is tiny (of order
of the inverse horizon radius). We give numerical evidences
indicating that this instability is caused by superradiance.Comment: 17 page
Universality of Highly Damped Quasinormal Modes for Single Horizon Black Holes
It has been suggested that the highly damped quasinormal modes of black holes
provide information about the microscopic quantum gravitational states
underlying black hole entropy. This interpretation requires the form of the
highly damped quasinormal mode frequency to be universally of the form:
, where is an integer, and is the
black hole temperature. We summarize the results of an analysis of the highly
damped quasinormal modes for a large class of single horizon, asymptotically
flat black holes.Comment: 9 pages, 1 figure, submitted to the proceedings of Theory CANADA 1,
which will be published in a special edition of the Canadian Journal of
Physic
Plasticity in the morphology of the fused frontals of Albanerpetontidae (Lissamphibia; Allocaudata)
Albanerpetontidae form an enigmatic extinct group of lissamphibians, ranging from the early Bathonian to the early Pleistocene. The Upper Jurassic outcrops of Portugal yield a large collection of material, suitable for addressing the intraspecific variation in and diagnostic potential of the characteristic fused frontals. We revise 58 specimens from the Guimarota beds of the Kimmeridgian Alcobaca Formation and describe 62 new frontal bones from the Kimmeridgian - Tithonian Lourinha Formation. Smaller specimens exhibit a vermicular dorsal ornamentation, while it is polygonal in larger specimens and other albanerpetontids. Compared to small specimens, larger specimens display: (1) larger ventrolateral crests extending posteriorly after the parietal margin; (2) a relatively shorter internasal process; (3) a frontal width across posterior edges relatively smaller; and (4) a ventromedian crest less pronounced. Morphometric analyses suggest a single species with different ontogenetic stages. Specimens are attributed to aff. Celtedens sp., based on a bell-shaped outline with a curved orbital margin (although variable in Portuguese specimens), and a flabellate, bulbous-shaped internasal process. The species is more similar to C. megacephalus than C. ibericus, but its phylogenetic position comprises an unresolved trichotomy. Our results show that intraspecific variation and homoplasy render the fused frontal non-diagnostic below the generic level
The Mystery of the Asymptotic Quasinormal Modes of Gauss-Bonnet Black Holes
We analyze the quasinormal modes of -dimensional Schwarzschild black holes
with the Gauss-Bonnet correction in the large damping limit and show that
standard analytic techniques cannot be applied in a straightforward manner to
the case of infinite damping. However, by using a combination of analytic and
numeric techniques we are able to calculate the quasinormal mode frequencies in
a range where the damping is large but finite. We show that for this damping
region the famous appears in the real part of the quasinormal mode
frequency. In our calculations, the Gauss-Bonnet coupling, , is taken
to be much smaller than the parameter , which is related to the black hole
mass.Comment: 12 pages and 5 figure
The Highly Damped Quasinormal Modes of Extremal Reissner-Nordstr\"om and Reissner-Nordstr\"om-de Sitter Black Holes
We analyze in detail the highly damped quasinormal modes of -dimensional
extremal Reissner-Nordstrm and
Reissner-Nordstrm-de Sitter black holes. We only consider the
extremal case where the event horizon and the Cauchy inner horizon coincide. We
show that, even though the topology of the Stokes/anti-Stokes lines in the
extremal case is different than the non-extremal case, the highly damped
quasinormal mode frequencies of extremal black holes match exactly with the
extremal limit of the non-extremal black hole quasinormal mode frequencies.Comment: 17 pages, 5 figure
Quasinormal modes of a black hole surrounded by quintessence
Using the third-order WKB approximation, we evaluate the quasinormal
frequencies of massless scalar field perturbation around the black hole which
is surrounded by the static and spherically symmetric quintessence. Our result
shows that due to the presence of quintessence, the scalar field damps more
rapidly. Moreover, we also note that the quintessential state parameter
(the ratio of pressure to the energy density ) play an
important role for the quasinormal frequencies. As the state parameter
increases the real part increases and the absolute value of the
imaginary part decreases. This means that the scalar field decays more slowly
in the larger quintessence case.Comment: 7 pages, 3 figure
Influence of Lorentz violation on Dirac quasinormal modes in the Schwarzschild black hole spacetime
Using the third-order WKB approximation and monodromy methods, we investigate
the influence of Lorentz violating coefficient (associated with a special
axial-vector field) on Dirac quasinormal modes in the Schwarzschild
black hole spacetime. At fundamental overtone, the real part decreases linearly
as the parameter increases. But the variation of the imaginary part with
becomes more complex. For the larger multiple moment , the magnitude of
imaginary part increases with the increase of , which means that presence of
Lorentz violation makes Dirac field damps more rapidly. At high overtones, it
is found that the real part of high-damped quasinormal frequency does not tend
to zero, which is quite a different from the symptotic Dirac quasinormal modes
without Lorentz violation.Comment: 10 pages, 4 figur
Area spectra of the rotating BTZ black hole from quasinormal modes
Following Bekenstein's suggestion that the horizon area of a black hole
should be quantized, the discrete spectrum of the horizon area has been
investigated in various ways. By considering the quasinormal mode of a black
hole, we obtain the transition frequency of the black hole, analogous to the
case of a hydrogen atom, in the semiclassical limit. According to Bohr's
correspondence principle, this transition frequency at large quantum number is
equal to classical oscillation frequency. For the corresponding classical
system of periodic motion with this oscillation frequency, an action variable
is identified and quantized via Bohr-Sommerfeld quantization, from which the
quantized spectrum of the horizon area is obtained. This method can be applied
for black holes with discrete quasinormal modes. As an example, we apply the
method for the both non-rotating and rotating BTZ black holes and obtain that
the spectrum of the horizon area is equally spaced and independent of the
cosmological constant for both cases
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