ar X iv : h ep - p h / 98 07 52 3 v 1 2 8 Ju l 1 99 8 VAND - TH - 98 - 12 The Warm Inflation
نویسنده
چکیده
The thermodynamics of inflationary expansion can be either isentropic or non-isentropic. Representing the early universe by a two fluid mixture of radiation energy density ρr and vacuum energy density ρv, the inflationary regime, when the scale factor accelerates R̈ > 0, is for ρv > ρr. From the point of view of two fluid Friedmann cosmology, isentropic inflationary expansion appears as a limiting case within the general regime of non-isentropic of inflation. In particle physics the vacuum equation of state ρv = −pv is realized by a scalar field with energy density ρ(φ) = φ̇/2 + (∇φ)/2 + V (φ), in which the potential energy density dominates
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