Standard-model particles and interactions from field equations on spin 9+1 dimensional space

We consider a Dirac equation set on an extended spin space that contains fermion and boson solutions. At given dimension, it determines the scalar symmetries. The standard field equations can be equivalently written in terms of such degrees of freedom, and are similarly constrained. At 9+1 dimensions, the SU(3) X SU(2)_L X U(1) gauge groups emerge, as well as solution representations with quantum numbers of related gauge bosons, leptons, quarks, Higgs-like particles and others as lepto-quarks. Information on the coupling constants is also provided; e. g., for the hypercharge g'=(1/2) sqrt(3/5) ~ >.387, at tree level.Comment: 13 pages, Fig. 1(a)-(d

Accelerated expansion of a universe containing a self-interacting Bose-Einstein gas

Acceleration of the universe is obtained from a model of non-relativistic particles with a short-range attractive interaction, at low enough temperature to produce a Bose-Einstein condensate. Conditions are derived for negative-pressure behavior. In particular, we show that a phantom-accelerated regime at the beginning of the universe solves the horizon problem, consistently with nucleosynthesis.Comment: 18 pages, 4 figure

Cosmology with dark energy decaying through its chemical-potential contribution

The consideration of dark energy's quanta, required also by thermodynamics, introduces its chemical potential into the cosmological equations. Isolating its main contribution, we obtain solutions with dark energy decaying to matter or radiation. When dominant, their energy densities tend asymptotically to a constant ratio, explaining today's dark energy-dark matter coincidence, and in agreement with supernova redshift data.Comment: 7 pages; presented at 2nd International Conference on Quantum Theories and Renormalization Group in Gravity and Cosmology, Barcelona, July, 200

Nuclei beyond the drip line

In a Thomas-Fermi model, calculations are presented for nuclei beyond the nuclear drip line at zero temperature. These nuclei are in equilibrium by the presence of an external gas, as may be envisaged in the astrophysical scenario. We find that there is a limiting asymmetry beyond which these nuclei can no longer be made stable.Comment: Physical Review C (in press), 1 ReVteX file for text, 4 PS-files for figure