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

Maity, Debaprasad; Saha, Pankaj

doi:10.1016/j.dark.2019.100317

Cited by 22 publications

(8 citation statements)

References 96 publications

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“…The inflationary predictions and dynamics of those models have been discussed in details in the work. The reheating constraints on the model through CMB and dark matter abundance has also been studied [17] considering the perturbative reheating phenomena. The study of perturbative reheating with a phenomenological term with inflaton decay constant Γ φ is simple and convenient to understand several important aspects of the reheating phase especially the connection between CMB and the present dark matter abundance through the reheating temperature.…”

Section: Jcap07(2019)018mentioning

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 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: Jcap07(2019)018mentioning

confidence: 99%

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

Maity

Saha

2019

J. Cosmol. Astropart. Phys.

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“…where we use Eq. (91). Due to the above expression of η −η f along with the fact that β ± (η f ) 2 1, the magnetic power spectrum during the reheating era becomes [29] ∂ρ( B)…”

Section: B Reheating With Time Independent Equation Of State: Evoluti...mentioning

confidence: 97%

“…In such scenario, the main idea is to parameterize the reheating phase by a constant effective equation of state. (iii) Finally we consider perturbative reheating scenario where the inflaton continuously decays into radiation and thus the effective equation of state during reheating becomes time dependent [83][84][85][86][87][88][89][90][91][92][93][94][95][96][97]. Because of the qualitative differences in the aforementioned two reheating scenarios, quantitatively different constraints on the effective theory as well as reheating parameters can be observed.…”

Section: Introductionmentioning

confidence: 99%

Effective Theory of Inflationary Magnetogenesis and Constraints on Reheating

Maity,

Pal,

Paul

2021

Preprint

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Effective theory framework based on symmetry has recently gained widespread interest in the field of cosmology. In this paper, we apply the same idea on the genesis of the primordial magnetic field and its evolution throughout the cosmological universe. Given the broken time-diffeomorphism symmetry by the cosmological background, we considered the most general Lagrangian of electromagnetic and metric fluctuation up to second order, which naturally breaks conformal symmetry in the electromagnetic (EM) sector. We also include parity violation in the electromagnetic sector with the motivation that has potential observational significance. In such a set-up, we explore the evolution of EM, scalar, and tensor perturbations considering different observational constraints. In our analysis we emphasize the role played by the intermediate reheating phase which has got limited interest in all the previous studies. Assuming the vanishing electrical conductivity during the entire period of reheating, the well-known Faraday electromagnetic induction has been shown to play a crucial role in enhancing the strength of the present-day magnetic field. We show how such physical effects combined with the PLANCK and the large scale magnetic field observation makes a large class of models viable and severely restricts the reheating equation of state parameter within a very narrow range of 0.01 < ω eff < 0.27, which is nearly independent of reheating scenarios we have considered.

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“…In this scenario, DM is produced out of thermal equilibrium via the so-called 'freeze-in' production mechanism. The interaction of the DM with the Standard Model (SM) particles in the freeze-in scenario needs to be extremely small such that they never attain a thermal equilibrium [11][12][13][14][15][16][17][18][19][20][21][22][23][24][25][26][27][28][29]. Such a tiny interaction strength makes freeze-in dark matter models challenging to detect at the experiments compared to the usual WIMP scenarios.…”

Section: Introductionmentioning

confidence: 99%

Fingerprints of freeze-in dark matter in an early matter-dominated era

Banerjee

Chowdhury

2022

SciPost Phys.

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We study the impact of an alternate cosmological history with an early matter-dominated epoch on the freeze-in production of dark matter. Such early matter domination is triggered by a meta-stable matter field dissipating into radiation. In general, the dissipation rate has a non-trivial temperature and scale factor dependence. Compared to the usual case of dark matter production via the freeze-in mechanism in a radiation-dominated universe, in this scenario, orders of magnitude larger coupling between the visible and the dark sector can be accommodated. Finally, as a proof of principle, we consider a specific model where the dark matter is produced by a sub-GeV dark photon having a kinetic mixing with the Standard Model photon. We point out that the parameter space of this model can be probed by the experiments in the presence of an early matter-dominated era.

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

Cited by 22 publications

References 96 publications

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

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

Effective Theory of Inflationary Magnetogenesis and Constraints on Reheating

Fingerprints of freeze-in dark matter in an early matter-dominated era

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