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

Maity, Debaprasad; Saha, Pankaj

doi:10.1088/1475-7516/2019/07/018

Cited by 44 publications

(28 citation statements)

References 80 publications

(148 reference statements)

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“…In a whole, this particular process comprises of unusual stochastic resonance production of lighter non relativistic particles, their further decays, backreaction in the presence of an expanding universe. Hence the estimate of the correct reheating temperature is more involved and requires rigorous lattice simulation [100,101]. Since we shall see in a while that this scenario turns out to be disfavoured due to overproduction of WIMP DM relic, we do not elaborate on this further.…”

Section: Reheatingmentioning

confidence: 99%

Cosmic inflation in minimal $$U(1)_{B-L}$$ model: implications for (non) thermal dark matter and leptogenesis

2021

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We study the possibility of realising cosmic inflation, dark matter (DM), baryon asymmetry of the universe (BAU) and light neutrino masses in non-supersymmetric minimal gauged $$B-L$$ B - L extension of the standard model with three right handed neutrinos. The singlet scalar field responsible for spontaneous breaking of $$B-L$$ B - L gauge symmetry also plays the role of inflaton by virtue of its non-minimal coupling to gravity. While the lightest right handed neutrino is the DM candidate, being stabilised by an additional $$Z_2$$ Z 2 symmetry, we show by performing a detailed renormalisation group evolution (RGE) improved study of inflationary dynamics that thermal DM is generally overproduced due to insufficient annihilations through gauge and scalar portals. This happens due to strict upper limits obtained on gauge and other dimensionless couplings responsible for DM annihilation while assuming the non-minimal coupling to gravity to be at most of order unity. The non-thermal DM scenario is viable, with or without $$Z_2$$ Z 2 symmetry, although in such a case the $$B-L$$ B - L gauge sector remains decoupled from the inflationary dynamics due to tiny couplings. We also show that the reheat temperature predicted by the model prefers non-thermal leptogenesis with hierarchical right handed neutrinos while being consistent with other requirements.

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Section: Reheatingmentioning

confidence: 99%

Cosmic inflation in minimal $$U(1)_{B-L}$$ model: implications for (non) thermal dark matter and leptogenesis

2021

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“…39). The equation of the inflaton fluctuations is identical to the one of the centred case (37), so the process of self-resonance remains unchanged. As discussed, it admits exponential solutions of the type δφ k ∼ e µ k u with Re[µ k ] > 0 for certain combinations of {κ, p}, which are described by the Floquet chart of Fig.…”

Section: B Analytical Analysis Of Resonances: Displaced Potentialmentioning

confidence: 99%

“…The inclusion of interactions to other field species can change the post-inflationary dynamics significantly. The evolution of the energy distribution and equation of state during preheating was studied in the case of quadraticquadratic inflaton-daughter field interactions in [36], and more extensively in [37] (see also [38] for a non-lattice study). The case of trilinear interactions was also considered in [39], and a case with higher order effective couplings in [40].…”

Section: Introductionmentioning

confidence: 99%

Characterizing the post-inflationary reheating history, Part I: single daughter field with quadratic-quadratic interaction

Antusch,

Figueroa,

Marschall

et al. 2021

Preprint

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We study the evolution of the energy distribution and equation of state of the Universe from the end of inflation until the onset of either radiation domination (RD) or a transient period of matter domination (MD). We use both analytical techniques and lattice simulations. We consider two-field models where the inflaton Φ has a monomial potential after inflation V (Φ) ∝ |Φ − v| p (p ≥ 2), and is coupled to a daughter field X through a quadratic-quadratic interaction g 2 Φ 2 X 2 . We consider two situations, depending on whether the potential has a minimum at i) v = 0, or ii) v > 0. In the scenario i), the final energy transferred to X is independent of g 2 and entirely determined by p: it is negligible for p < 4, and of order ∼ 50% for p ≥ 4. The system goes to MD at late times for p = 2, while it goes to RD for p > 2. In the later case, we can calculate exactly the number of e-folds until RD as a function of g 2 , and hence predict accurately inflationary observables like the scalar tilt ns and the tensor-to-scalar ratio r. In the scenario ii), the energy is always transferred completely to X for p > 2, as long as its effective mass m 2 X = g 2 (Φ − v) 2 is not negligible. For p = 2, the final ratio between the energy densities of X and Φ depends strongly on g 2 . For all p ≥ 2, the system always goes to MD at late times.

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“…On the other hand, through Eq. ( 37) and the covariant conservation equation, we can relate ρ re with the energy density ρ e at the end of inflation 1+wa) , (39) with the number of e-folds N re characterizing the duration of the reheating period and…”

Section: End Of Inflation and Reheatingmentioning

confidence: 99%

Higher-order extension of Starobinsky inflation: initial conditions, slow-roll regime, and reheating phase

Rodrigues-da-Silva,

Bezerra-Sobrinho,

Medeiros

2021

Preprint

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The most current observational data corroborate the Starobinsky model as one of the strongest candidates in the description of an inflationary regime. Motivated by such success, extensions of the Starobinsky model have been increasingly recurrent in the literature. The theoretical justification for this is well grounded: higher-order gravities arise in high-energy physics in the search for the ultraviolet completeness of general relativity. In this paper, we propose to investigate the inflation due to the extension of the Starobinsky model characterized by the inclusion of the R 3 term. We make a complete analysis of the potential and phase space of the model, where we observe the existence of three regions with distinct dynamics for the scalar field. We can establish restrictive limits for the number of e-folds through a study of the reheating and by considering the usual couplings of the standard matter fields and gravity. Thereby, we duly confront our model with the observational data from Planck, BICEP3/Keck, and BAO. Finally, we discuss how the inclusion of the cubic term restricts the initial conditions necessary for the occurrence of a physical inflation.

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

Cited by 44 publications

References 80 publications

Cosmic inflation in minimal $$U(1)_{B-L}$$ model: implications for (non) thermal dark matter and leptogenesis

Cosmic inflation in minimal $$U(1)_{B-L}$$ model: implications for (non) thermal dark matter and leptogenesis

Characterizing the post-inflationary reheating history, Part I: single daughter field with quadratic-quadratic interaction

Higher-order extension of Starobinsky inflation: initial conditions, slow-roll regime, and reheating phase

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