It is shown that curvature effects, though completely negligible at the present day, can drastically alter thermal spectra at early times in some inflationary cosmological models. This can lead to a modification of the thermal history of the universe before the entropy production. The effects are only present for spatially curved k ≠ 0 Robertson-Walker models, not for spatially flat k = 0 models. If the entropy increase is >> 10^87 and k ≠ 0 then the energy density in the quantum fields is much greater, and hence the universe is much younger, at the onset of inflation than would be the case in a spatially flat universe. The effect is not relevant for chaotic inflation
In the standard inflationary paradigm, the seeds for cosmic structures are assumed to be of quantum ...
An energetic justification of a thermal component during inflation is given. The thermal component c...
The trace of the stress-energy tensor of the cosmological fluid, proportional to the Ricci scalar cu...
It is shown that curvature effects, though completely negligible at the present day, can drastically...
Curvature effects in inflationary Robertson-Walker models, although neg ligible at the present day, ...
textGravitational waves are truly transparent to matter in the Universe and carry the information of...
In cosmological scenarios with thermal inflation, extra eras of moduli matter domination, thermal in...
If the spatial curvature of the universe at the beginning of inflation is negative, there is an enha...
We propose a model for early universe cosmology without the need for fundamental scalar fields. Cosm...
It is shown that gravitating magnetic fields affect the evolution of curvature perturbations in a wa...
If the universe had a large curvature before inflation there is a deviation from the scale invariant...
Non-flat Friedmann-Lemaitre models solving the horizon problem in which, prior to and during inflati...
Abstract: Inflation creates large-scale cosmological density perturbations that are characterized by...
A new model of thermal inflation is introduced, in which the mass of the thermal waterfall field is ...
We propose a model for early universe cosmology without the need for fundamental scalar fields. Cosm...
In the standard inflationary paradigm, the seeds for cosmic structures are assumed to be of quantum ...
An energetic justification of a thermal component during inflation is given. The thermal component c...
The trace of the stress-energy tensor of the cosmological fluid, proportional to the Ricci scalar cu...
It is shown that curvature effects, though completely negligible at the present day, can drastically...
Curvature effects in inflationary Robertson-Walker models, although neg ligible at the present day, ...
textGravitational waves are truly transparent to matter in the Universe and carry the information of...
In cosmological scenarios with thermal inflation, extra eras of moduli matter domination, thermal in...
If the spatial curvature of the universe at the beginning of inflation is negative, there is an enha...
We propose a model for early universe cosmology without the need for fundamental scalar fields. Cosm...
It is shown that gravitating magnetic fields affect the evolution of curvature perturbations in a wa...
If the universe had a large curvature before inflation there is a deviation from the scale invariant...
Non-flat Friedmann-Lemaitre models solving the horizon problem in which, prior to and during inflati...
Abstract: Inflation creates large-scale cosmological density perturbations that are characterized by...
A new model of thermal inflation is introduced, in which the mass of the thermal waterfall field is ...
We propose a model for early universe cosmology without the need for fundamental scalar fields. Cosm...
In the standard inflationary paradigm, the seeds for cosmic structures are assumed to be of quantum ...
An energetic justification of a thermal component during inflation is given. The thermal component c...
The trace of the stress-energy tensor of the cosmological fluid, proportional to the Ricci scalar cu...