30,812 research outputs found
Linearisation instability of gravity waves?
Gravity waves in irrotational dust spacetimes are characterised by nonzero
magnetic Weyl tensor . In the linearised theory, the divergence of
is set to zero. Recently Lesame et al. [Phys. Rev. D {\bf 53}, 738
(1996)] presented an argument to show that, in the exact nonlinear theory, forces , thus implying a linearisation instability for gravity
waves interacting with matter. However a sign error in the equations
invalidates their conclusion. Bianchi type V spacetimes are shown to include
examples with . An improved covariant formalism is used to
show that in a generic irrotational dust spacetime, the covariant constraint
equations are preserved under evolution. It is shown elsewhere that \mbox{div}
H=0 does not generate further conditions.Comment: 8 pages Revtex; to appear Phys. Rev.
Consistency of dust solutions with div H=0
One of the necessary covariant conditions for gravitational radiation is the
vanishing of the divergence of the magnetic Weyl tensor H_{ab}, while H_{ab}
itself is nonzero. We complete a recent analysis by showing that in
irrotational dust spacetimes, the condition div H=0 evolves consistently in the
exact nonlinear theory.Comment: 3 pages Revte
Exact non-equilibrium solutions of the Einstein-Boltzmann equations. II
We find exact solutions of the Einstein-Boltzmann equations with relaxational
collision term in FRW and Bianchi I spacetimes. The kinematic and thermodynamic
properties of the solutions are investigated. We give an exact expression for
the bulk viscous pressure of an FRW distribution that relaxes towards
collision-dominated equilibrium. If the relaxation is toward collision-free
equilibrium, the bulk viscosity vanishes - but there is still entropy
production. The Bianchi I solutions have zero heat flux and bulk viscosity, but
nonzero shear viscosity. The solutions are used to construct a realisation of
the Weyl Curvature Hypothesis.Comment: 16 pages LaTex, CQG documentstyle (ioplppt
Exploring CP Violation in the MSSM
We explore the prospects for observing CP violation in the minimal
supersymmetric extension of the Standard Model (MSSM) with six CP-violating
parameters, three gaugino mass phases and three phases in trilinear soft
supersymmetry-breaking parameters, using the CPsuperH code combined with a
geometric approach to maximize CP-violating observables subject to the
experimental upper bounds on electric dipole moments. We also implement
CP-conserving constraints from Higgs physics, flavour physics and the upper
limits on the cosmological dark matter density and spin-independent scattering.
We study possible values of observables within the constrained MSSM (CMSSM),
the non-universal Higgs model (NUHM), the CPX scenario and a variant of the
phenomenological MSSM (pMSSM). We find values of the CP-violating asymmetry
A_CP in b -> s gamma decay that may be as large as 3%, so future measurements
of A_CP may provide independent information about CP violation in the MSSM. We
find that CP-violating MSSM contributions to the B_s meson mass mixing term
Delta M_Bs are in general below the present upper limit, which is dominated by
theoretical uncertainties. If these could be reduced, Delta M_Bs could also
provide an interesting and complementary constraint on the six CP-violating
MSSM phases, enabling them all to be determined experimentally, in principle.
We also find that CP violation in the h_{2,3} tau+ tau- and h_{2,3} tbar t
couplings can be quite large, and so may offer interesting prospects for future
pp, e+ e-, mu+ mu- and gamma gamma colliders.Comment: 36 pages, 32 figure
Integrability of irrotational silent cosmological models
We revisit the issue of integrability conditions for the irrotational silent
cosmological models. We formulate the problem both in 1+3 covariant and 1+3
orthonormal frame notation, and show there exists a series of constraint
equations that need to be satisfied. These conditions hold identically for
FLRW-linearised silent models, but not in the general exact non-linear case.
Thus there is a linearisation instability, and it is highly unlikely that there
is a large class of silent models. We conjecture that there are no spatially
inhomogeneous solutions with Weyl curvature of Petrov type I, and indicate
further issues that await clarification.Comment: Minor corrections and improvements; 1 new reference; to appear Class.
Quantum Grav.; 16 pages Ioplpp
Constraints on Inflationary Solutions in the Presence of Shear and Bulk Viscosity
Inflationary models and their claim to solve many of the outstanding problems
in cosmology have been the subject of a great deal of debate over the last few
years. A major sticking point has been the lack of both good observational and
theoretical arguments to single out one particular model out of the many that
solve these problems. Here we examine the degree of restrictiveness on the
dynamical relationship between the cosmological scale factor and the inflation
driving self-interaction potential of a minimally coupled scalar field, imposed
by the condition that the scalar field is required to be real during a
classical regime (the reality condition). We systema\-tically look at the
effects of this constraint on many of the inflationary models found in the
literature within the FLRW framework, and also look at what happens when
physically motivated perturbations such as shear and bulk viscosity are
introduced. We find that in many cases, either the models are totally excluded
or the reality condition gives rise to constraints on the scale factor and on
the various parameters of the model.Comment: 21 pages, LaTe
Dynamics of Inflationary Universes with Positive Spatial Curvature
If the spatial curvature of the universe is positive, then the curvature term
will always dominate at early enough times in a slow-rolling inflationary
epoch. This enhances inflationary effects and hence puts limits on the possible
number of e-foldings that can have occurred, independently of what happened
before inflation began and in particular without regard for what may have
happened in the Planck era. We use a simple multi-stage model to examine this
limit as a function of the present density parameter and the epoch
when inflation ends.Comment: 9 Pages RevTex4. Revised and update
Aberration of the Cosmic Microwave Background
The motion of the solar system barycenter with respect to the cosmic
microwave background (CMB) induces a very large apparent dipole component into
the CMB brightness map at the 3 mK level. In this Letter we discuss another
kinematic effect of our motion through the CMB: the small shift in apparent
angular positions due to the aberration of light. The aberration angles are
only of order beta ~0.001, but this leads to a potentially measurable
compression (expansion) of the spatial scale in the hemisphere toward (away
from) our motion through the CMB. In turn, this will shift the peaks in the
acoustic power spectrum of the CMB by a factor of order 1 +/- beta. For current
CMB missions, and even those in the foreseeable future, this effect is small,
but should be taken into account. In principle, if the acoustic peak locations
were not limited by sampling noise (i.e., the cosmic variance), this effect
could be used to determine the cosmic contribution to the dipole term.Comment: 3 pages, 1 figure, comments welcome. Submitted to ApJ Letter
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