Reheating constraints on a two-field inflationary model

Asadi, Kosar; Nozari, Kourosh

doi:10.1016/j.nuclphysb.2019.114827

Cited by 15 publications

(12 citation statements)

References 43 publications

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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%

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Two-Field Inflationary Model and Swampland de Sitter Conjecture

Gashti¹

2021

Preprint

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In this paper, we are going to investigate a new perspective of the two-field inflation model with respect to the swampland dS conjecture. At the first step, we study the two-fields inflation model, and apply the swampland conjecture to our model. Then, we calculate some cosmological parameters such as scalar spectrum index, tensor-to-scalar ratio, and compare our results with the recent observational data. Also, we give numerical analysis to show agreement with observational data.

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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%

“…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%

Two-Field Inflationary Model and Swampland de Sitter Conjecture

Gashti¹

2021

Preprint

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“…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%

Power spectrum of density fluctuations, halo abundances and clustering with primordial black holes

Padilla,

Magana,

Sureda

et al. 2020

Preprint

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We calculate the effect of dark matter (DM) being encapsulated in primordial black holes (PBHs) on the power spectrum of density fluctuations P (k); we also look at its effect on the abundance of haloes and their clustering. We adopt a growth of Poisson fluctuations that starts only after the moment of matter and radiation equality and study both monochromatic and extended Press-Schechter distributions. We present updated monochromatic black hole mass constraints by demanding < 10% deviations from the Λ cold dark matter power spectrum at a scale of k = 1hMpc −1 . Our results show that PBHs with masses > 10 4 h −1 M are excluded from conforming all of the dark matter in the Universe; they would, however, be able to act as seeds for super massive black holes if they conform a small fraction of the DM. We also apply this condition to our extended Press-Schechter (PS) mass functions, and find that the Poisson power is scale dependent even before applying evolution, due to the change of the mass density in PBHs with redshift, and therefore with scale, as they start affecting the gravitational potential at different times. We find that characteristic masses M * ≤ 10 2 h −1 M are allowed, leaving only two characteristic PBH mass windows of PS mass functions when combining with previous constraints, at M * ∼ 10 2 h −1 M and ∼ 10 −8 h −1 M where all of the DM can be in PBHs. The resulting dark matter halo mass functions within these windows are similar to those resulting from cold dark matter made of fundamental particles, but as soon as the parameters produce unrealistic P (k), the resulting halo mass functions and their bias as a function of halo mass deviate strongly from the behaviour measured in the real Universe.

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“…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%

Preheating and Reheating after Standard Inflation

Bourakadi¹

2021

Preprint

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We study the two-phase scenario following inflation, where the initial step is preheating, accompanied by a step of perturbative reheating at which inflaton field decays transferring all of its energy to create relativistic particles, the interaction of these particles will evolve towards a state of thermal equilibrium with a temperature T re called the reheating temperature. It is observed that the scenario of reheating normally predicts the maximum reheating temperature that corresponds to an almost instantaneous transition from inflation to the radiation domination era. This will naturally lead to a nonperturbative preheating. In this framework, we propose constraints on the reheating duration parameters expressed in terms of the cosmic microwave background (CMB) inflationary scalar spectral index. In this work we study the compatibility of polynomial and Higgs models of inflation with the observational data obtained from Planck 2018.

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Reheating constraints on a two-field inflationary model

Cited by 15 publications

References 43 publications

Two-Field Inflationary Model and Swampland de Sitter Conjecture

Two-Field Inflationary Model and Swampland de Sitter Conjecture

Power spectrum of density fluctuations, halo abundances and clustering with primordial black holes

Preheating and Reheating after Standard Inflation

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