Quasi-thermal Universe and its implications for gravitino production, baryogenesis and dark matter

Details Quasi-thermal Universe and its implications for gravitino production, baryogenesis and dark matter Quasi-thermal Universe and its implications for gravitino production, baryogenesis and dark matter

2005-05-06

arxiv.org/abs/hep-ph/0505050v3

Physics

High Energy Physics

High Energy Physics - Phenomenology

Title changed. Upon requests the role of SUSY flat directions in thermalization is emphasized. Minor changes and added comment

Scientific paper

Under general circumstances full thermal equilibrium may not be established for a long period after perturbative or non-perturbative decay of the inflaton has completed. One can instead have a distribution of particles which is in kinetic equilibrium and evolves adiabatically during this period. Number-violating reactions which are required to establish chemical equilibrium can become efficient only at much later times. We highlight some of the striking consequences of such a quasi-thermal Universe. In particular, thermal gravitino production yields {\it no bound} on the maximum temperature of the primordial thermal bath alone. As another consequence, the lower bound on the mass of the lightest right-handed (s)neutrino from thermal leptogenesis can be $\gg 10^{9}$ GeV. Depending on the phase, a Wino or Higgsino considerably lighter than TeV, or a Bino in the bulk region, can be a viable {\it thermal} dark matter candidate. Finally the electroweak symmetry may never be restored in the early Universe, therefore weakening any hopes of realizing a successful electroweak baryogenesis.

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