Minimal plateau inflationary cosmologies and constraints from reheating

Maity, Debaprasad; Saha, Pankaj

doi:10.1088/1361-6382/ab0038

Cited by 21 publications

(16 citation statements)

References 109 publications

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“…In this work we have studied the preheating and subsequent thermalization after minimal plateau inflation introduced in our earlier work [16]. These class of models are parameterized by the power n of the inflaton field φ and most importantly a scale φ * that controls the energy scale of inflation, similar to the α parameter for α-attractor models.…”

Section: Introductionmentioning

confidence: 99%

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(P)reheating after minimal plateau inflation and constraints from CMB

Maity

Saha

2019

J. Cosmol. Astropart. Phys.

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In this paper we have investigated the preheating phase for a class of plateau inflationary model considering the four-legs interaction term (1/2)g 2 φ 2 χ 2 between the inflaton (φ) and reheating field (χ). We specifically focus on the effects of our model parameter φ * which controls inflationary dynamics. For φ * < M p , the departure of the inflaton potential from the usual power-law behavior φ n significantly modifies the microscopic behavior of the preheating dynamics. We analyze and compare the efficiency of production, thermalization behavior and the final equation of states of the system for different values of n = 2, 4, 6 considering two different values of φ * . Most importantly as we increase n, or decrease φ * , the preheating occurs very efficiently with the final equation of state to be that of the radiation, w = 1/3. However, for n = 2, the final equation of state turned out to be w 0.2. In the non-perturbative framework complete decay of inflaton could not be achieved with the four-legs interaction for any model under consideration. Therefore, in order to complete the reheating process, we perform the perturbative analysis for the second stage of the reheating phase. With the appropriate initial condition set by the non-perturbative dynamics, we solved a set of homogeneous Boltzmann equations for both the fields supplemented by the constraints coming from the subsequent entropy conservation. In so doing, we calculated the reheating temperature which was otherwise ill-defined right after the end of preheating. The temperature can be uniquely fixed for a given inflaton decay constant and the CMB temperature. We also compare our results with the conventional reheating constraint analysis and discuss the limits on the inflaton decay constant from the field theory perspective.

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Section: Introductionmentioning

confidence: 99%

“…In this section we will briefly describe the minimal plateau inflationary model and its characteristics introduced in [16]. We have already explained in our previous work, considering a simple power-law potential φ n , we can obtain our general class of non-polynomial form of the potential given as…”

Section: A Brief Introduction To the Minimal Inflation Modelmentioning

confidence: 99%

(P)reheating after minimal plateau inflation and constraints from CMB

Maity

Saha

2019

J. Cosmol. Astropart. Phys.

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“…In this paper, we have done the reheating constraint analysis in detail for a class of inflationary models with non-standard potential [21]. Our focus was on understanding the inflation model as well as dark matter phenomenology via reheating phase.…”

Section: Discussionmentioning

confidence: 99%

“…In this section we will briefly describe the inflationary models proposed in [21]. The model is a non-polynomial modification to the usual power-law chaotic potentials φ n and is given by,…”

Section: A Brief Account On Minimal Plateau Inflationary Potentialsmentioning

confidence: 99%

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CMB constraints on dark matter phenomenology via reheating in minimal plateau inflation

Maity

Saha

2019

Physics of the Dark Universe

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We consider the CMB constrains on reheating and dark matter parameter space for a specific plateau type inflationary model. The plateau inflationary models which are currently most favored models from data can be well approximated by a potential of the form V (φ) ∝ φ n around φ = 0. This fact makes it possible to study the reheating phase with general inflaton equation of state in a viable cosmological scenario. In addition, following our recent work[1], we generalize the connection between reheating and the present CMB data and the dark matter parameter space for general inflaton equation of state parameter.

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