ar X iv : g r - qc / 0 11 10 09 v 1 4 N ov 2 00 1 Torsion Gravity Effects on Charged - Particle and Neutron Interferometers

ar X iv : g r - qc / 0 01 11 12 v 1 3 0 N ov 2 00 0 GROUP AVERAGING AND REFINED ALGEBRAIC QUANTIZATION : WHERE ARE WE NOW ?

Refined Algebraic Quantization and Group Averaging are powerful methods for quantizing constrained systems. They give constructive algorithms for generating observables and the physical inner product. This work outlines the current status of these ideas with an eye toward quantum gravity. The main goal is provide a description of outstanding problems and possible research topics in the field.

ar X iv : 0 71 1 . 25 73 v 1 [ gr - q c ] 1 6 N ov 2 00 7 Spinning particles in scalar - tensor gravity

We develop a new model of a spinning particle in Brans-Dicke space-time using a metric-compatible connection with torsion. The particle's spin vector is shown to be Fermi-parallel (by the Levi-Civita connection) along its worldline (an autoparallel of the metric-compatible connection) when neglecting spin-curvature coupling.

ar X iv : g r - qc / 0 51 11 56 v 1 2 9 N ov 2 00 5 Adiabatic Particle Production with Decaying Λ and Anisotropic Universe

The inclusion of cosmological constant into Einstein field equation was done primarily by Einstein himself with a view to model a static universe. Later he discarded the cosmological constant (and commented [1] “...... the biggest blunder of my life”), on the basis of the observational data supporting the expansion of the universe. Subsequently, it was reintroduced and then omitted to match wit...

ar X iv : g r - qc / 0 11 20 12 v 1 7 D ec 2 00 1 RELATIVISTIC GRAVITY WITH A DYNAMICAL PREFERRED FRAME

ar X iv : g r - qc / 0 61 10 12 v 1 2 N ov 2 00 6 The Energy of Bianchi Type I and II Universes in Teleparallel Gravity

For certain models, the energy of the universe which includes the energy of both the matter and the gravitational fields is obtained by using the quasilocal energy-momentum in teleparallel gravity. It is shown that in the case of the Bianchi type I and II universes, not only the total energy but also the quasilocal energy-momentum for any region vanishes independently of the three dimen-sionles...