299 research outputs found
Relativistic Dynamics of Vector Bosons in the Field of Gravitational Radiation
We consider a model of the state evolution of relativistic vector bosons,
which includes both the dynamical equations for the particle four-velocity and
the equations for the polarization four-vector evolution in the field of a
nonlinear plane gravitational wave. In addition to the gravitational minimal
coupling, tidal forces linear in curvature tensor are suggested to drive the
particle state evolution. The exact solutions of the evolutionary equations are
obtained. Birefringence and tidal deviations from the geodesic motion are
discussed.Comment: 10 pages, no figures, Te
Spin-axion coupling
We establish a new covariant phenomenological model, which describes an
influence of pseudoscalar (axion) field on spins of test massive particles. The
model includes general relativistic equations of particle motion and spin
evolution in background pseudoscalar (axion), electromagnetic and gravitational
fields. It describes both the direct spin-axion coupling of the gradient type
and indirect spin-axion interaction mediated by electromagnetic fields. Special
attention is paid to the direct spin-axion coupling caused by the gradient of
the pseudoscalar (axion) field. We show that it describes a spin precession,
when the pseudoscalar (axion) field is inhomogeneous and/or non-stationary.
Applications of the model, which correspond to the three types of four-vectors
attributed to the gradient of the pseudoscalar (axion) field (time-like,
space-like, and null), are considered in detail. These are the spin precessions
induced by relic cosmological axions, axions distributed around spherically
symmetric static objects, and axions in a gravitational wave field,
respectively. We discuss features of the obtained exact solutions and some
general properties of the axionically induced spin rotation.Comment: 15 pages; replaced with the version accepted for publication in Phys.
Rev. D; new Subsection IVB and 13 references are adde
Dark Energy: A Unifying View
Different models of the cosmic substratum which pretend to describe the
present stage of accelerated expansion of the Universe like the CDM
model or a Chaplygin gas, can be seen as special realizations of a holographic
dark energy cosmology if the option of an interaction between pressurless dark
matter and dark energy is taken seriously. The corresponding interaction
strength parameter plays the role of a cosmological constant. Differences occur
at the perturbative level. In particular, the pressure perturbations are
intrinsically non-adiabatic.Comment: 9 pages, selected for "Honorable Mention" by the Gravity Research
Foundatio
Non-minimal coupling for the gravitational and electromagnetic fields: A general system of equations
We establish a new self-consistent system of equations for the gravitational
and electromagnetic fields. The procedure is based on a non-minimal non-linear
extension of the standard Einstein-Hilbert-Maxwell action. General properties
of a three-parameter family of non-minimal linear models are discussed. In
addition, we show explicitly, that a static spherically symmetric charged
object can be described by a non-minimal model, second order in the derivatives
of the metric, when the susceptibility tensor is proportional to the
double-dual Riemann tensorComment: 15 page
Archimedean-type force in a cosmic dark fluid: II. Qualitative and numerical study of a multistage Universe expansion
In this (second) part of the work we present the results of numerical and
qualitative analysis, based on a new model of the Archimedean-type interaction
between dark matter and dark energy. The Archimedean-type force is linear in
the four-gradient of the dark energy pressure and plays a role of
self-regulator of the energy redistribution in a cosmic dark fluid. Because of
the Archimedean-type interaction the cosmological evolution is shown to have a
multistage character. Depending on the choice of the values of the model
guiding parameters,the Universe's expansion is shown to be perpetually
accelerated, periodic or quasiperiodic with finite number of
deceleration/acceleration epochs. We distinguished the models, which can be
definitely characterized by the inflation in the early Universe, by the
late-time accelerated expansion and nonsingular behavior in intermediate
epochs, and classified them with respect to a number of transition points.
Transition points appear, when the acceleration parameter changes the sign,
providing the natural partition of the Universe's history into epochs of
accelerated and decelerated expansion. The strategy and results of numerical
calculations are advocated by the qualitative analysis of the instantaneous
phase portraits of the dynamic system associated with the key equation for the
dark energy pressure evolution.Comment: 15 pages, 12 figures, Part II, typos corrected, Fig.4 replaced,
references correcte
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