752 research outputs found
Hawking Radiation as Tunneling through the Quantum Horizon
Planck-scale corrections to the black-hole radiation spectrum in the
Parikh-Wilczek tunneling framework are calculated. The corrective terms arise
from modifications in the expression of the surface gravity in terms of the
mass-energy of the black hole-emitted particle system. The form of the new
spectrum is discussed together with the possible consequences for the fate of
black holes in the late stages of evaporation.Comment: 13 pages; the contents of this paper overlap somewhat with the
earlier submissions hep-th/0504188 and gr-qc/0505015; (v2) references added
and various cosmetic (but no physics) changes, to appear in JHE
On the Existence of the Logarithmic Correction Term in Black Hole Entropy-Area Relation
In this paper we consider a model universe with large extra dimensions to
obtain a modified black hole entropy-area relation. We use the generalized
uncertainty principle to find a relation between the number of spacetime
dimensions and the presence or vanishing of logarithmic prefactor in the black
hole entropy-area relation. Our calculations are restricted to the
microcanonical ensembles and we show that in the modified entropy-area
relation, the microcanonical logarithmic prefactor appears only when spacetime
has an even number of dimensions.Comment: 9 Pages, No Figure
Symmetries at stationary Killing horizons
It has often been suggested (especially by Carlip) that spacetime symmetries
in the neighborhood of a black hole horizon may be relevant to a statistical
understanding of the Bekenstein-Hawking entropy. A prime candidate for this
type of symmetry is that which is exhibited by the Einstein tensor. More
precisely, it is now known that this tensor takes on a strongly constrained
(block-diagonal) form as it approaches any stationary, non-extremal Killing
horizon. Presently, exploiting the geometrical properties of such horizons, we
provide a particularly elegant argument that substantiates this highly
symmetric form for the Einstein tensor. It is, however, duly noted that, on
account of a "loophole", the argument does fall just short of attaining the
status of a rigorous proof.Comment: 11 pages, Revte
Strings and the Holographic Description of Asymptotically de Sitter Spaces
Asymptotically de Sitter spaces can be described by Euclidean boundary
theories with entropies given by the modified Cardy--Verlinde formula. We show
that the Cardy--Verlinde formula describes a string with a rescaled tension
which in fact is a string at the stretched cosmological horizon as seen from
the boundary. The temperature of the boundary theory is the rescaled Hagedorn
temperature of the string. Our results agree with an alternative description of
asymptotically de Sitter spaces in terms of strings on the stretched horizon.
The relation between the two descriptions is given by the large gravitational
redshift between the boundary and the stretched horizon and a shift in energy.Comment: 15 pages in phyzzx.tex, minor correction
Numeričko predviđanje izobličenja nakon zavarivanja s različnim slijedom zavarivanja i spajanja
Welding simulation of a test cover for hydropower plant was made due to very large dimensions of the cover. The main aim was to predict distortion after welding in order to avoid machining the cover. Welding process was simulated with the Sysweld program to keep distortion in desired limits. Various welding sequences and clamping conditions were calculated to reduce the distortion. Calculation of microstructure constituents in virtual complex geometry of joints was also analyzed.Simulacija zavarivanja testnog pokrova hidroelektrane provedena je zbog velikih dimenzija ispitne prevlake. Osnovni je cilj predvidjeti izobličenje nakon zavarivanja. Radi postizanja veličine izobličenja u željenim granicama proces zavarivanja je simuliran programom Sysweld. Različiti tijekovi zavarivanja i uvjeta spajanja prorač unati su radi smanjenja izobličenja. Određivanje mikrostrukturnih konstituenata u virtualnoj komleksnoj geometriji spojeva je također provedeno
Entropy Corrections for Schwarzschild and Reissner-Nordstr\"om Black Holes
Schwarzschild black hole being thermodynamically unstable, corrections to its
entropy due to small thermal fluctuations cannot be computed. However, a
thermodynamically stable Schwarzschild solution can be obtained within a cavity
of any finite radius by immersing it in an isothermal bath. For these boundary
conditions, classically there are either two black hole solutions or no
solution. In the former case, the larger mass solution has a positive specific
heat and hence is locally thermodynamically stable. We find that the entropy of
this black hole, including first order fluctuation corrections is given by:
{\cal S} = S_{BH} - \ln[\f{3}{R} (S_{BH}/4\p)^{1/2} -2]^{-1} + (1/2)
\ln(4\p), where is its Bekenstein-Hawking entropy and is the
radius of the cavity. We extend our results to four dimensional
Reissner-Nordstr\"om black holes, for which the corresponding expression is:
{\cal S} = S_{BH} - \f{1}{2} \ln [ {(S_{BH}/\p R^2) ({3S_{BH}}/{\p R^2} -
2\sqrt{{S_{BH}}/{\p R^2 -\a^2}}) \le(\sqrt{{S_{BH}}/{\p R^2}} - \a^2 \ri)}/
{\le({S_{BH}}/{\p R^2} -\a^2 \ri)^2} ]^{-1} +(1/2)\ln(4\p). Finally, we
generalise the stability analysis to Reissner-Nordstr\"om black holes in
arbitrary spacetime dimensions, and compute their leading order entropy
corrections. In contrast to previously studied examples, we find that the
entropy corrections in these cases have a different character.Comment: 6 pages, Revtex. References added, minor changes. Version to appear
in Class. Quant. Gra
Dynamical Instability of Self-Tuning Solution with Antisymmetric Tensor Field
We consider the dynamical stability of a static brane model that incorporates
a three-index antisymmetric tensor field and has recently been proposed as a
possible solution to the cosmological constant problem. Ultimately, we are able
to establish the existence of time-dependent, purely gravitational
perturbations. As a consequence, the static solution of interest is
``dangerously'' located at an unstable saddle point. This outcome is suggestive
of a hidden fine tuning in what is an otherwise self-tuning model.Comment: 16 Pages, Latex; Discussion added but conclusions unchange
Obrazovanje faze AlFeSi u slitini AlSi12 s dodatkom cera
The influence of cerium addition on the solidification sequence and microstructure constituents of the Al-Si alloys with 12,6 mass % Si was examined. The solidification was analyzed by a simple thermal analysis. The microstructures were examined with conventional light and scanning electron microscopy. Ternary AlSiCe phase was formed in the Al-Si alloys with added cerium during the solidification process. AlSiCe and β-AlFeSi phases solidified together in the region that solidified the last. Cerium addition influenced on the morphology of the α-AlFeSi phase solidification.Ispitan je utjecaj dodatka cera na tijek skrućivanja i oblikovanje mikrostrukture u Al-Si slitini s 12,6 mas. % Si. Skrućivanje je praćeno s jednostavnom toplinskom analizom. Mikrostrukture su kvantificirane pomoću svjetlosnog i elektronskog mikroskopa. Pri skrućivanju Al-Si slitine s dodatkom Ce, obrazuju se faze Al-SiCe, AlSiCe te β-AlFeSi, koje se skrućivaju zajedno u završnom području skrućivanja. Dodatak Ce utječe na morfologiju skrućivanja faze α-AlFeSi
Delocalization of brane gravity by a bulk black hole
We investigate the analogue of the Randall-Sundrum brane-world in the case
when the bulk contains a black hole. Instead of the static vacuum Minkowski
brane of the RS model, we have an Einstein static vacuum brane. We find that
the presence of the bulk black hole has a dramatic effect on the gravity that
is felt by brane observers. In the RS model, the 5D graviton has a stable
localized zero-mode that reproduces 4D gravity on the brane at low energies.
With a bulk black hole, there is no such solution -- gravity is delocalized by
the 5D horizon. However, the brane does support a discrete spectrum of
metastable massive bound states, or quasinormal modes, as was recently shown to
be the case in the RS scenario. These states should dominate the high frequency
component of the bulk gravity wave spectrum on a cosmological brane. We expect
our results to generalize to any bulk spacetime containing a Killing horizon.Comment: 7 pages, 6 figure
Thermal Fluctuations and Black Hole Entropy
In this paper, we consider the effect of thermal fluctuations on the entropy
of both neutral and charged black holes. We emphasize the distinction between
fixed and fluctuating charge systems; using a canonical ensemble to describe
the former and a grand canonical ensemble to study the latter. Our novel
approach is based on the philosophy that the black hole quantum spectrum is an
essential component in any such calculation. For definiteness, we employ a
uniformly spaced area spectrum, which has been advocated by Bekenstein and
others in the literature. The generic results are applied to some specific
models; in particular, various limiting cases of an (arbitrary-dimensional)
AdS-Reissner-Nordstrom black hole. We find that the leading-order quantum
correction to the entropy can consistently be expressed as the logarithm of the
classical quantity. For a small AdS curvature parameter and zero net charge, it
is shown that, independent of the dimension, the logarithmic prefactor is +1/2
when the charge is fixed but +1 when the charge is fluctuating.We also
demonstrate that, in the grand canonical framework, the fluctuations in the
charge are large, , even when .
A further implication of this framework is that an asymptotically flat,
non-extremal black hole can never achieve a state of thermal equilibrium.Comment: 25 pages, Revtex; references added and corrected, and some minor
change
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