4,754 research outputs found
Rippled Cosmological Dark Matter from Damped Oscillating Newton Constant
Let the reciprocal Newton 'constant' be an apparently non-dynamical
Brans-Dicke scalar field damped oscillating towards its General Relativistic
VEV. We show, without introducing additional matter fields or dust, that the
corresponding cosmological evolution averagely resembles, in the Jordan frame,
the familiar dark radiation -> dark matter -> dark energy domination sequence.
The fingerprints of our theory are fine ripples, hopefully testable, in the FRW
scale factor; they die away at the General Relativity limit. The possibility
that the Brans-Dicke scalar also serves as the inflaton is favorably examined.Comment: RevTex4, 12 pages, 5 figures; Minor revision, References adde
Codimension Two Branes in Einstein-Gauss-Bonnet Gravity
Codimension two branes play an interesting role in attacking the cosmological
constant problem. Recently, in order to handle some problems in codimension two
branes in Einstein gravity, Bostock {\it et al.} have proposed using
six-dimensional Einstein-Gauss-Bonnet (EGB) gravity instead of six-dimensional
Einstein gravity. In this paper, we present the solutions of codimension two
branes in six-dimensional EGB gravity. We show that Einstein's equations take a
"factorizable" form for a factorized metric tensor ansatz even in the presence
of the higher-derivative Gauss-Bonnet term. Especially, a new feature of the
solution is that the deficit angle depends on the brane geometry. We discuss
the implication of the solution to the cosmological constant problem. We also
comment on a possible problem of inflation model building on codimension two
branes.Comment: 16 pages, no figures. v2: References added; v3: Reference added,
Sec.4 and 5 combined into one; v4: References added, minor corrections, to
appear in Physical Review
Geometrical Constraints on the Cosmological Constant
The cosmological constant problem is examined under the assumption that the
extrinsic curvature of the space-time contributes to the vacuum. A compensation
mechanism based on a variable cosmological term is proposed. Under a suitable
hypothesis on the behavior of the extrinsic curvature, we find that an
initially large rolls down rapidly to zero during the early stages
of the universe. Using perturbation analysis, it is shown that such vacuum
behaves essentially as a spin-2 field which is independent of the metric.Comment: [email protected], 17 pages, Latex, 2 figures obtained by reques
Transition between phantom and non-phantom phases with time dependent cosmological constant and Cardy-Verlinde formula
We investigate the transition phenomenon of the universe between a phantom
and a non-phantom phases. Particular attention is devoted to the case in which
the cosmological constant depends on time and is proportional to the square of
the Hubble parameter. Inhomogeneous equations of state are used and the
equation of motion is solved. We find that, depending on the choice of the
input parameters, the universe can transit from the non-phantom to the phantom
phase leading to the appearance of singularities. In particular, we find that
the phantom universe ends in the singularity of type III, unlike the case
without variable cosmological constant in which the phantom phase ends
exclusively in the big rip (singularity of type I). The Cardy-Verlinde formula
is also introduced for inhomogeneous equation of state and we find that its
equivalence with the total entropy of the universe, coming from the Friedmann
equations, occurs only for special choice of the input parameter at the
present time.Comment: 12 pages, 2 figure
Thermodynamics of Decaying Vacuum Cosmologies
The thermodynamic behavior of vacuum decaying cosmologies is investigated
within a manifestly covariant formulation. Such a process corresponds to a
continuous irreversible energy flow from the vacuum component to the created
matter constituents. It is shown that if the specific entropy per particle
remains constant during the process, the equilibrium relations are preserved.
In particular, if the vacuum decays into photons, the energy density and
average number density of photons scale with the temperature as and . The temperature law is determined and a generalized
Planckian type form of the spectrum, which is preserved in the course of the
evolution, is also proposed. Some consequences of these results for decaying
vacuum FRW type cosmologies as well as for models with ``adiabatic'' photon
creation are discussed.Comment: 21 pages, uses LATE
Induced Lorentz- and CPT-violating Chern-Simons term in QED: Fock-Schwinger proper time method
Using the Fock-Schwinger proper time method, we calculate the induced
Chern-Simons term arising from the Lorentz- and CPT-violating sector of quantum
electrodynamics with a term. Our
result to all orders in coincides with a recent linear-in- calculation
by Chaichian et al. [hep-th/0010129 v2]. The coincidence was pointed out by
Chung [Phys. Lett. {\bf B461} (1999) 138] and P\'{e}rez-Victoria [Phys. Rev.
Lett. {\bf 83} (1999) 2518] in the standard Feynman diagram calculation with
the nonperturbative-in- propagator.Comment: 11 pages, no figur
Lorentz and CPT symmetries in commutative and noncommutative spacetime
We investigate the fermionic sector of a given theory, in which massive and
charged Dirac fermions interact with an Abelian gauge field, including a non
standard contribution that violates both Lorentz and CPT symmetries. We offer
an explicit calculation in which the radiative corrections due to the fermions
seem to generate a Chern-Simons-like effective action. Our results are obtained
under the general guidance of dimensional regularization, and they show that
there is no room for Lorentz and CPT violation in both commutative and
noncommutative spacetime.Comment: RevTex4, 7 pages, to be published in J. Phys.
Spheres, Deficit Angles and the Cosmological Constant
We consider compactifications of six dimensional gravity in four dimensional
Minkowski or de Sitter space times a two dimensional sphere, S^2. As has been
recently pointed out, it is possible to introduce 3-branes in these backgrounds
with arbitrary tension without affecting the effective four dimensional
cosmological constant, since its only effect is to induce a deficit angle in
the sphere. We show that if a monopole like configuration of a 6D U(1) gauge
field is used to produce the spontaneous compactification of the two extra
dimensions in a sphere a fine tuning between brane and bulk parameters is
reintroduced once the quantization condition for the gauge field is taken into
account, so the 4D cosmological constant depends on the brane tension. This
problem is absent if instead of the monopole we consider a four form field
strength in the bulk to obtain the required energy-momentum tensor. Also,
making use of the four form field, we generalize the solution to an arbitrary
number of dimensions (\ge 6), keeping always four noncompact dimensions and
compactifying the rest in a n-dimensional sphere. We show that a (n+1)-brane
with arbitrary tension can be introduced in this background without affecting
the effective 4D cosmological constant.Comment: 14 pages, LaTe
Relating the thermodynamic arrow of time to the causal arrow
Consider a Hamiltonian system that consists of a slow subsystem S and a fast
subsystem F. The autonomous dynamics of S is driven by an effective
Hamiltonian, but its thermodynamics is unexpected. We show that a well-defined
thermodynamic arrow of time (second law) emerges for S whenever there is a
well-defined causal arrow from S to F and the back-action is negligible. This
is because the back-action of F on S is described by a non-globally Hamiltonian
Born-Oppenheimer term that violates the Liouville theorem, and makes the second
law inapplicable to S. If S and F are mixing, under the causal arrow condition
they are described by microcanonic distributions P(S) and P(S|F). Their
structure supports a causal inference principle proposed recently in machine
learning.Comment: 10 page
Understanding Radiatively Induced Lorentz-CPT Violation in Differential Regularization
We have investigated the perturbative ambiguity of the radiatively induced
Chern-Simons term in differential regularization. The result obtained in this
method contains all those obtained in other regularization schemes and the
ambiguity is explicitly characterized by an indefinite ratio of two
renormalization scales. It is argued that the ambiguity can only be eliminated
by either imposing a physical requirement or resorting to a more fundamental
principle. Some calculation techniques in coordinate space are developed in the
appendices.Comment: RevTex, 14 pages, one figure drawn by FEYNMAN, several references are
modified and a paragraph about a general choice on the mass scales is added
in page
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