2,071 research outputs found
Some solutions of linearized 5-d gravity with brane
We consider linearized 5-d gravity in the Randall-Sundrum brane world. The
class of static solutions for linearized Einstein equations is found. Also we
obtaine wave solutions describing radiation from an imaginary point source
located at the Planck distance from the brane. We analyze the fields asymptotic
behavior and peculiarities of matter sources.Comment: Latex, 8 page
Precursors, black holes, and a locality bound
We revisit the problem of precursors in the AdS/CFT correspondence.
Identification of the precursors is expected to improve our understanding of
the tension between holography and bulk locality and of the resolution of the
black hole information paradox. Previous arguments that the precursors are
large, undecorated Wilson loops are found to be flawed. We argue that the role
of precursors should become evident when one saturates a certain locality
bound. The spacetime uncertainty principle is a direct consequence of this
bound.Comment: 26 pages, 8 figs; reference added, minor clarification in sec. 2;
incorrect draft mistakenly used in version
Fluctuating geometries, q-observables, and infrared growth in inflationary spacetimes
Infrared growth of geometrical fluctuations in inflationary spacetimes is
investigated. The problem of gauge-invariant characterization of growth of
perturbations, which is of interest also in other spacetimes such as black
holes, is addressed by studying evolution of the lengths of curves in the
geometry. These may either connect freely falling "satellites," or wrap
non-trivial cycles of geometries like the torus, and are also used in
diffeomorphism- invariant constructions of two-point functions of field
operators. For spacelike separations significantly exceeding the Hubble scale,
no spacetime geodesic connects two events, but one may find geodesics
constrained to lie within constant-time spatial slices. In inflationary
geometries, metric perturbations produce significant and growing corrections to
the lengths of such geodesics, as we show in both quantization on an inflating
torus and in standard slow-roll inflation. These become large, signaling
breakdown of a perturbative description of the geometry via such observables,
and consistent with perturbative instability of de Sitter space. In particular,
we show that the geodesic distance on constant time slices during inflation
becomes non-perturbative a few e-folds after a given scale has left the
horizon, by distances \sim 1/H^3 \sim RS, obstructing use of such geodesics in
constructing IR-safe observables based on the spatial geometry. We briefly
discuss other possible measures of such geometrical fluctuations.Comment: 33 pages, 2 figures, latex; v2: typos corrected, references improve
Comments on information loss and remnants
The information loss and remnant proposals for resolving the black hole
information paradox are reconsidered. It is argued that in typical cases
information loss implies energy loss, and thus can be thought of in terms of
coupling to a spectrum of ``fictitious'' remnants. This suggests proposals for
information loss that do not imply planckian energy fluctuations in the low
energy world. However, if consistency of gravity prevents energy
non-conservation, these remnants must then be considered to be real. In either
case, the catastrophe corresponding to infinite pair production remains a
potential problem. Using Reissner-Nordstrom black holes as a paradigm for a
theory of remnants, it is argued that couplings in such a theory may give
finite production despite an infinite spectrum. Evidence for this is found in
analyzing the instanton for Schwinger production; fluctuations from the
infinite number of states lead to a divergent stress tensor, spoiling the
instanton calculation. Therefore naive arguements for infinite production fail.Comment: 30 pages (harvmac l mode) UCSBTH-93-35 (minor reference and typo
corrections
Numerical Analysis of Black Hole Evaporation
Black hole formation/evaporation in two-dimensional dilaton gravity can be
described, in the limit where the number of matter fields becomes large, by
a set of second-order partial differential equations. In this paper we solve
these equations numerically. It is shown that, contrary to some previous
suggestions, black holes evaporate completely a finite time after formation. A
boundary condition is required to evolve the system beyond the naked
singularity at the evaporation endpoint. It is argued that this may be
naturally chosen so as to restore the system to the vacuum. The analysis also
applies to the low-energy scattering of -wave fermions by four-dimensional
extremal, magnetic, dilatonic black holes.Comment: 10 pages, 9 figures in separate uuencoded fil
Non-uniform Braneworld Stars: an Exact Solution
The first exact interior solution to Einstein's field equations for a static
and non-uniform braneworld star with local and non-local bulk terms is
presented. It is shown that the bulk Weyl scalar is always
negative inside the stellar distribution, in consequence it reduces both the
effective density and the effective pressure. It is found that the anisotropy
generated by bulk gravity effect has an acceptable physical behaviour inside
the distribution. Using a Reissner-N\"{o}rdstrom-like exterior solution, the
effects of bulk gravity on pressure and density are found through matching
conditions.Comment: 22 pages, 3 figures, version to be published in International Journal
of Modern Physics D (IJMPD
A global picture of quantum de Sitter space
Perturbative gravity about a de Sitter background motivates a global picture
of quantum dynamics in `eternal de Sitter space,' the theory of states which
are asymptotically de Sitter to both future and past. Eternal de Sitter physics
is described by a finite dimensional Hilbert space in which each state is
precisely invariant under the full de Sitter group. This resolves a
previously-noted tension between de Sitter symmetry and finite entropy.
Observables, implications for Boltzmann brains, and Poincare recurrences are
briefly discussed.Comment: 17 pages, 1 figure. v2: minor changes, references added. v3: minor
changes to correspond to PRD versio
p-Branes and the GZK Paradox
In spacetimes with asymmetric extra dimensions, cosmic neutrino interactions
may be extraordinarily enhanced by p-brane production. Brane formation and
decay may then initiate showers deep in the Earth's atmosphere at rates far
above the standard model rate. We explore the p-brane discovery potential of
cosmic ray experiments. The absence of deeply penetrating showers at AGASA
already provides multi-TeV bounds on the fundamental Planck scale that
significantly exceed those obtained from black hole production in symmetric
compactification scenarios. This sensitivity will be further enhanced at the
Auger Observatory. We also examine the possibility that p-brane formation
resolves the GZK paradox. For flat compactifications, astrophysical bounds
exclude this explanation. For warped scenarios, a solution could be consistent
with the absence of deep showers only for extra dimensions with fine-tuned
sizes well below the fundamental Planck length. In addition, it requires
moderately penetrating showers, so far not reported, and ~100% modifications to
standard model phenomenology at 100 GeV energies.Comment: 8 pages, 6 figure
Quasilocalized gravity without asymptotic flatness
We present a toy model of a generic five-dimensional warped geometry in which
the 4D graviton is not fully localized on the brane. Studying the tensor sector
of metric perturbation around this background, we find that its contribution to
the effective gravitational potential is of 4D type (1/r) at the intermediate
scales and that at the large scales it becomes 1/r^{1+alpha}, 0<alpha=< 1 being
a function of the parameters of the model (alpha=1 corresponds to the
asymptotically flat geometry). Large-distance behavior of the potential is
therefore not necessarily five-dimensional. Our analysis applies also to the
case of quasilocalized massless particles other than graviton.Comment: 9 pages, 1 figure; to be published in Phys. Rev.
- …