Effects of a preinflation radiation-dominated epoch to CMB anisotropy

Wang, I-Chin; Ng, Kin-Wang

doi:10.1103/physrevd.77.083501

Cited by 55 publications

(82 citation statements)

References 28 publications

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“…For example in Refs. [6,7], a radiation-dominated pre-inflationary era was considered and in [8], a pre-inflation matter era provided by primordial micro black hole remnants was introduced. The CMB quadruple anomaly affects the lowest modes of the primordial power spectrum; i.e.…”

Section: Introductionmentioning

confidence: 99%

Slow-roll inflation preceded by a topological defect phaseà laChaplygin gas

et al. 2013

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We present a simple toy model corresponding to a network of frustrated topological defects of domain walls or cosmic strings that exist previous to the standard slow-roll inflationary era of the universe. Such a network (i) can produce a slower inflationary era than that of the standard scenario if it corresponds to a network of frustrated domain walls or (ii) can induce a vanishing universal acceleration; i.e., the universe would expand at a constant speed, if it corresponds to a network of frustrated cosmic strings. Those features are phenomenologically modeled by a Chaplygin gas that can interpolate between a network of frustrated topological defects and a de Sitter-like or a powerlaw inflationary era. We show that this scenario can alleviate the quadruple anomaly of the cosmic microwave background spectrum. Using the method of the Bogoliubov coefficients, we obtain the spectrum of the gravitational waves as would be measured today for the whole range of frequencies. We comment on the possible detection of this spectrum by the planned detectors like BBO and DECIGO.PACS numbers: 98.80. Bp, 95.36.+x

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Section: Introductionmentioning

confidence: 99%

Slow-roll inflation preceded by a topological defect phaseà laChaplygin gas

et al. 2013

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“…Expression (19) shows that including α-dependent terms lead to decreasing of entropy similarly as we have in the case with β-terms only. To calculate the heat capacity of a black hole we use a well-known thermodynamical relation:…”

Section: Entropy and Heat Capacity Of A Black Holementioning

confidence: 84%

Microscopic Black Hole and Uncertainty Principle With Minimal Length and Momentum

Stetsko

2013

Int. J. Mod. Phys. A

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We investigate a microscopic black hole in case of modified generalized uncertainty principle with a minimal uncertainty in position as well as in momentum. We calculate thermodynamical functions of a Schwarzschild black hole such as temperature, entropy and heat capacity. It is shown that incorporation of minimal uncertainty in momentum leads to minimal temperature of a black hole. Minimal temperature gives rise to appearance of a phase transition. Emission rate equation and black hole's evaporation time are also obtained.

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“…[17]). We point out that there also exist good theoretical reasons for considering models of "just enough inflation" in which δN is small.…”

Section: Introductionmentioning

confidence: 99%

“…[9][10][11][12][13][14][15][16][17] consider the possibility that the inflaton too could have been in thermal equilibrium during the pre-inflationary radiation era, as has been discussed above. In the scenario of Ref.…”

Section: Introductionmentioning

confidence: 99%

Constraints on just enough inflation preceded by a thermal era

et al. 2016

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If the inflationary era is preceded by a radiation dominated era in which the inflaton too was in thermal equilibrium at some very early time then the CMB data places an upper bound on the comoving temperature of the (decoupled) inflaton quanta. In addition, if one considers models of "just enough" inflation, where the number of e-foldings of inflation is just enough to solve the horizon and flatness problems, then we get a lower bound on the Hubble parameter during inflation, H inf , which is in severe conflict with the upper bound from tensor perturbations. Alternatively, imposing the upper bound on H inf implies that such scenarios are compatible with the data only if the number of relativistic degrees of freedom in the thermal bath in the pre-inflationary Universe is extremely large (greater than 10 9 or 10 11 ). We are not aware of scenarios in which this can be satisfied.

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Effects of a preinflation radiation-dominated epoch to CMB anisotropy

Cited by 55 publications

References 28 publications

Slow-roll inflation preceded by a topological defect phaseà laChaplygin gas

Slow-roll inflation preceded by a topological defect phaseà laChaplygin gas

Microscopic Black Hole and Uncertainty Principle With Minimal Length and Momentum

Constraints on just enough inflation preceded by a thermal era

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