Noncommutative field gas driven inflation

We investigate early time inflationary scenarios in a Universe filled with a dilute noncommutative bosonic gas at high temperature. A noncommutative bosonic gas is a gas composed of a bosonic scalar field with noncommutative field space on a commutative spacetime. Such noncommutative field theories...

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Bibliographic Details
Published inJournal of cosmology and astroparticle physics Vol. 2008; no. 4; p. 005
Main Authors Barosi, Luciano, Brito, Francisco A, Queiroz, Amilcar R
Format Journal Article
LanguageEnglish
Published United States IOP Publishing 01.04.2008
Subjects
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS
COMMUTATION RELATIONS
CPT THEOREM
DISPERSION RELATIONS
ENERGY DENSITY
EQUATIONS OF STATE
FIELD THEORIES
INFLATIONARY UNIVERSE
LORENTZ INVARIANCE
QUANTUM MECHANICS
SCALAR FIELDS
SPACE-TIME
TEMPERATURE RANGE 0400-1000 K
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Summary:We investigate early time inflationary scenarios in a Universe filled with a dilute noncommutative bosonic gas at high temperature. A noncommutative bosonic gas is a gas composed of a bosonic scalar field with noncommutative field space on a commutative spacetime. Such noncommutative field theories were recently introduced as a generalization of quantum mechanics on a noncommutative spacetime. Key features of these theories are Lorentz invariance violation and CPT violation. In the present study we use a noncommutative bosonic field theory that, besides the noncommutative parameter {theta}, shows up a further parameter {sigma}. This parameter {sigma} controls the range of the noncommutativity and acts as a regulator for the theory. Both parameters play a key role in the modified dispersion relations of the noncommutative bosonic field, leading to possible striking consequences for phenomenology. In this work we obtain an equation of state p = {omega}({sigma},{theta};{beta}){rho} for the noncommutative bosonic gas relating pressure p and energy density {rho}, in the limit of high temperature. We analyse possible behaviours for these gas parameters {sigma}, {theta} and {beta}, so that -1{<=}{omega}<-1/3, which is the region where the Universe enters an accelerated phase.
ISSN:1475-7516
1475-7516
DOI:10.1088/1475-7516/2008/04/005