Thermal inflation and the moduli problem
Sep, 199528 pages
Published in:
- Phys.Rev.D 53 (1996) 1784-1798
e-Print:
- hep-ph/9510204 [hep-ph]
Report number:
- LANCS-TH-9505,
- RESCEU-16-95,
- LANCASTER-TH-9505
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Abstract:
In supersymmetric theories a field can develop a vacuum expectation value M \gg 10~3\GeV, even though its mass is of order to 10~3\GeV. The finite temperature in the early Universe can hold such a field at zero, corresponding to a false vacuum with energy density . When the temperature falls below , the thermal energy density becomes negligible and an era of thermal inflation begins. It ends when the field rolls away from zero at a temperature of order , corresponding to of order 10 -folds of inflation which does not affect the density perturbation generated during ordinary inflation. Thermal inflation can solve the Polonyi/moduli problem if is within one or two orders of magnitude of 10~{12}\GeV. Parametric resonance may lead to rapid partial reheating giving a high enough temperature for a variety of methods of baryogenesis. One can also have double thermal inflation which can solve the Polonyi/moduli problem even more efficiently.- grand unified theory
- supersymmetry
- astrophysics
- inflation
- finite temperature
- potential: flat direction
- effective potential
- moduli space
- bibliography
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