21 research outputs found
CMB Fluctuation Amplitude from Dark Energy Partitions
It is assumed that the dark energy observed today is frozen as a result of a
phase transition involving the source of that energy. Postulating that the dark
energy de-coherence which results from this phase transition drives statistical
variations in the energy density specifies a class of cosmological models in
which the cosmic microwave background (CMB) fluctuation amplitude at last
scattering is approximately .Comment: 7 Pages, Poster presented at Texas@Stanford conference, Dec. 2004,
minor clarification
A Non-Perturbative, Finite Particle Number Approach to Relativistic Scattering Theory
We present integral equations for the scattering amplitudes of three scalar
particles, using the Faddeev channel decomposition, which can be readily
extended to any finite number of particles of any helicity. The solution of
these equations, which have been demonstrated to be calculable, provide a
non-perturbative way of obtaining relativistic scattering amplitudes for any
finite number of particles that are Lorentz invariant, unitary, cluster
decomposable and reduce unambiguously in the non-relativistic limit to the
non-relativistic Faddeev equations. The aim of this program is to develop
equations which explicitly depend upon physically observable input variables,
and do not require renormalization or dressing of these parameters to connect
them to the boundary states
Evidence for a Cosmological Phase Transition on the TeV Scale
Examining the reverse evolution of the universe from the present, long before
reaching Planck density dynamics one expects major modifications from the
de-coherent thermal equations of state, suggesting a prior phase that has
macroscopic coherence properties. The assumption that the phase transition
occurs during the radiation dominated epoch, and that zero-point motions drive
the fluctuations associated with this transition, specifies a class of
cosmological models in which the cosmic microwave background fluctuation
amplitude at last scattering is approximately . Quantum measurability
constraints (eg. uncertainly relations) define cosmological scales whose
expansion rates can be at most luminal. Examination of these constraints for
the observed dark energy density establishes a time interval from the
transition to the present. It is shown that the dark energy can consistently be
interpreted as due to the vacuum energy of collective gravitational modes which
manifest as the zero-point motions of coherent Planck scale mass units prior to
the gravitational quantum de-coherence of the cosmology. A scenario is
suggested that connects microscopic physics to the relevant cosmological scale.Comment: 35 page
Construction of Non-Perturbative, Unitary Particle-Antiparticle Amplitudes for Finite Particle Number Scattering Formalisms
Starting from a unitary, Lorentz invariant two-particle scattering amplitude
, we show how to use an identification and replacement process to construct a
unique, unitary particle-antiparticle amplitude. This process differs from
conventional on-shell Mandelstam s,t,u crossing in that the input and
constructed amplitudes can be off-diagonal and off-energy shell. Further,
amplitudes are constructed using the invariant parameters which are appropriate
to use as driving terms in the multi-particle, multichannel non-perturbative,
cluster decomposable, relativistic scattering equations of the Faddeev-type
integral equations recently presented by Alfred, Kwizera, Lindesay and Noyes.
It is therefore anticipated that when so employed, the resulting multi-channel
solutions will also be unitary. The process preserves the usual
particle-antiparticle symmetries. To illustrate this process, we construct a
J=0 scattering length model chosen for simplicity. We also exhibit a class of
physical models which contain a finite quantum mass parameter and are Lorentz
invariant. These are constructed to reduce in the appropriate limits, and with
the proper choice of value and sign of the interaction parameter, to the
asymptotic solution of the non-relativistic Coulomb problem, including the
forward scattering singularity, the essential singularity in the phase, and the
Bohr bound-state spectrum