2019
DOI: 10.1016/j.nuclphysb.2019.114827
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Reheating constraints on a two-field inflationary model

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Cited by 15 publications
(12 citation statements)
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“…Concerning the above equation and scale factor α(t), the Friedmann equations for the evolution of α(t) are as follows [69],…”
Section: Two-field Inflation Modelmentioning
confidence: 99%
See 1 more Smart Citation
“…Concerning the above equation and scale factor α(t), the Friedmann equations for the evolution of α(t) are as follows [69],…”
Section: Two-field Inflation Modelmentioning
confidence: 99%
“…According to the above concepts and using the Hamilton-Jacobi equation, and also the description of inflation dynamics, we consider the following form of Hubble parameter [69],…”
Section: Two-field Inflation Modelmentioning
confidence: 99%
“…However, a different model for reaheating after Inflation such that reheating ends at larger scale factors can dramatically increase fm for FCT (e.g. Kuroyanagi et al 2014;Cook et al 2015;German 2020;Asadi & Nozari 2019) and alleviate this possible issue. Because of this we consider both HC and FCT scenarios in their two forms referred to generically by fm = 1 and min(fm).…”
Section: Pbh Formation At Fixed Conformal Time and At Horizon Crossingmentioning
confidence: 99%
“…We, therefore, will take into account the maximum reheating temperature that leads to the lower values of N re wich favor a much higher e-folds number of preheating, and prove that it's parameterized by a post-inflationary e-folds N pre . The equation of state (eos) ω is an important parameter that can be used in the study of the evolution of the universe, the (eos) takes different values in each era of its history, for example, ω ≥ −1/3 is needed to end inflation [8,9] but during the reheating the (eos) increase from 0 to 1/3, where ω = 1/3 corresponds to a universe of the radiation domination era [7].…”
Section: Introductionmentioning
confidence: 99%