

Ashtekar and Samuel have shown that Bianchi cosmological
models with compact spatial sections must be of Bianchi
class A. Motivated by general results on the symmetry
reduction of variational principles, we show how to extend
the Ashtekar-Samuel results to the setting of weakly locally
homogeneous spaces as defined, e.g., by Singer and
Thurston. More precisely, it is shown that any
m-dimensional homogeneous space G/K admitting a
G-invariant volume form admits a compact discrete quotient
only if the Lie algebra cohomology of G relative to K is
non-vanishing at degree m.
[D8.002] Power-laws from critical gravitiational collapse: The mass distribution of subsolar objects
Nicolas Yunes (The Pennsylvania State University), Matt Visser (Victoria University of Wellington)
At large mass, the initial mass function [IMF], which
describes the size distribution of stellar objects, is
characterized by a power-law with the Salpeter exponent. At
small [substellar] mass, theory indicates that there must be
some change in this power law. Indeed, direct observation
indicates that the IMF is certainly modified below
approximately one-tenth of a solar mass. We demonstrate that
at very low mass the IMF should again be given by a power
law with an exponent opposite in sign to the high-mass
exponent. Furthermore, we verify that this low-mass exponent
is in principle calculable via dynamical systems theory
applied to gravitational collapse. Observational data
indicate a broad agreement with the sign of the low-mass
exponent, and a preponderance of evidence pointing to a
critical mass-scaling exponent approximately equal to two.
[D8.003] Higher-Derivative Palatini Gravity and the Accelerating Universe
Lior Burko, Paolo Gondolo (University of Utah)
It has been suggested that higher-derivative gravity could give a classical explanation to the observed acceleration of the Universe. Others have objected, citing inconsistencies with solar-system observations.
It was recently noted that when higher-derivative gravity is obtained through the Palatini variational principle, the resulting theory is no longer in conflict with solar-system observations. A controversy has started on the question of consistency with certain laboratory electron scattering experiments.
In my talk I will note that any higher-derivative Palatini
theory is necessarily non-metric. Specifically, if particles
are assumed to move along geodesics, the mass of particles
is not conserved. Although Lorentz-invariance violations may
be too small to be detected in the laboratory, they may have
observable effects at the cosmological scale.
[D8.004] The Kerr-Schild Method in 2+1 Gravity
Leda Pena (Universidad Tecnologica Metropolitana), Nelson Zamorano (Universidad de Chile)
The Kerr-Schild method has proved to be a powerful tool for
generating many of the most recurrent solutions of Einstein
equations. We show here that this method works with the same
efficiency in (2+1) dimensions. Our examples are the BTZ
metric and the magnetic solution in (2 + 1) gravity. In both
cases we have reobtained the known solutions and extended
them to include new ones that contain charge and angular
momentum. Following the same thread, we have extended the
Dray and t'Hooft solution to this lower dimension case. This
exact solution of Einstein equations, includes a null
particle travelling along the event horizon of a black hole.
These results underline the unifying character of this
approach, several solutions of Einstein equations find their
way through this formalism. Also, the simplicity of this
approach and the existence of programs for algebraic
manipulation of the Einstein equations overcome the main
difficulty of this method: the physical interpretation of
the resulting equations.
[D8.005] The Schwarzschild solution in the DGP model
Chad Middleton, George Siopsis (University of Tennessee)
We discuss the Schwarzschild solution in the
Dvali-Gabadadze-Porrati (DGP) model. We obtain two different
perturbative expansions which are valid in two distinct
domains, respectively, separated by a critical radius. We
show that this critical radius can be determined by the
lowest-order contributions to the two perturbative
expansions. At large distances, the solution is the standard
solution of the linearized Einstein equations obtained by
DGP. At distances below the critical radius on the brane,
the perturbative expansion yields the four-dimensional
Schwarzschild solution. This is similar to the Vainshtein
solution in massive gravity demonstrating the absence of the
van Dam-Veltman-Zakharov (vDVZ) discontinuity.
[D8.006] Perturbative calculation of quasi-normal modes of Schwarzschild black holes
George Siopsis (University of Tennessee), Suphot Musiri (Srinakharinwiroth University)
We discuss a systematic method of analytically calculating
the asymptotic form of quasi-normal frequencies of a
four-dimensional Schwarzschild black hole by expanding
around the zeroth-order approximation to the wave equation
proposed by Motl and Neitzke. We obtain an explicit
expression for the first-order correction and arbitrary
spin. Our results are in agreement with the results from WKB
and numerical analyses in the case of scalar and
gravitational waves.
[D8.007] The Newtonian Mercury Perihelion, Light Bending and General Relativity
Ronald Kotas (Grand Quantum Research)
The 43 arc seconds per century of Mercury's perihelion advance (3.8 x 10 ^-12 of the total) are accounted for by an Electromagnetic, Gravitational coupling function respective to the precise 2/3 ratio of day-to-year of Mercury and \textbfNuclear Quantum Gravitation^\copyright . The slight rotation and the drag of the other planets cause the Sun's Electromagnetic domains-fields to rotate-change that small amount. This is absolutely a Newtonian, \textbfNuclear Quantum Gravitation^\copyright effect and not a General Relativity effect. General Relativity cannot have an effect at a distance from a gravitating body. There has been no proven mechanism of this. Fallacy tensors and time-space do not produce tangible results. They do not function. Further, General Relativity fails the Cavendish experiment. Where in the equations of General Relativity is there the ability for two bodies of any size to attract each other? Other so-called proofs of General Relativity such as light bending near the Sun are also incorrect and false.