Toward an effective field theory approach to reheating

Özsoy, Ogan; Giblin, John T.; Nesbit, Eva; Şengör, Gizem; Watson, Scott

doi:10.1103/physrevd.96.123524

Cited by 20 publications

(39 citation statements)

References 82 publications

(256 reference statements)

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“…III, see Eqs. (11), (14), agrees well with the lattice simulations (Fig. 11) when the first narrow instability band plays an important role.…”

Section: Duration To Radiation Dominationsupporting

confidence: 79%

“…For M ∼ m Pl , ΔN rad is given by Eqs. (11) and (14). Note that with δ ≈ 0.126 → 0.1, ΔN br → ΔN rad .…”

Section: Observational Implications For Inflationary Observablesmentioning

confidence: 97%

“…Thus, ΔN rad and ρ end =ρ rad are bounded from above and these bounds can be calculated from the parameters of the inflationary potential. Even if additional relativistic species are coupled to the inflaton, 14 our calculated ΔN rad and ρ end =ρ rad are robust upper bounds. The lower bound is of course ΔN rad ¼ 0 and ρ end =ρ rad ¼ 1.…”

mentioning

confidence: 99%

“…In particular, self-resonance, where the homogeneous inflaton condensate pumps energy into its own fluctuations, can lead to interesting nonlinear effects even in absence of couplings to other fields (e.g., [23][24][25]). Such explosive particle production, formation of nontopological and topological solitons (e.g., [23,26]), as well as relics such as black holes (e.g., [27]) and primordial gravitational waves (e.g., [28][29][30]), amongst others, make 1 See [12][13][14] for attempts at some model-independent approaches. reheating an exciting dynamical playground.…”

Section: Introductionmentioning

confidence: 99%

“…Our bounds on the expansion history after inflation, reduce the uncertainties in N ⋆ significantly and hence in the predictions for the two CMB observables, as can be seen in the figures. 14 As long the decay is perturbative to avoid metastable, nonlinear states.…”

mentioning

confidence: 99%

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Self-resonance after inflation: Oscillons, transients, and radiation domination

2018

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Homogeneous oscillations of the inflaton after inflation can be unstable to small spatial perturbations even without coupling to other fields. We show that for inflaton potentials ∝ jϕj 2n near jϕj ¼ 0 and flatter beyond some jϕj ¼ M, the inflaton condensate oscillations can lead to self-resonance, followed by its complete fragmentation. We find that for nonquadratic minima (n > 1), shortly after backreaction, the equation of state parameter, w → 1=3. If M ≪ m Pl , radiation domination is established within less than an e-fold of expansion after the end of inflation. In this case self-resonance is efficient and the condensate fragments into transient, localised spherical objects which are unstable and decay, leaving behind them a virialized field with mean kinetic and gradient energies much greater than the potential energy. This end-state yields w ¼ 1=3. When M ∼ m Pl we observe slow and steady, self-resonance that can last many e-folds before backreaction eventually shuts it off, followed by fragmentation and w → 1=3. We provide analytical estimates for the duration to w → 1=3 after inflation, which can be used as an upper bound (under certain assumptions) on the duration of the transition between the inflationary and the radiation dominated states of expansion. This upper bound can reduce uncertainties in CMB observables such as the spectral tilt n s , and the tensor-to-scalar ratio r. For quadratic minima (n ¼ 1), w → 0 regardless of the value of M. This is because when M ≪ m Pl , long-lived oscillons form within an e-fold after inflation, and collectively behave as pressureless dust thereafter. For M ∼ m Pl , the self-resonance is inefficient and the condensate remains intact (ignoring longterm gravitational clustering) and keeps oscillating about the quadratic minimum, again implying w ¼ 0.

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“…III, see Eqs. (11), (14), agrees well with the lattice simulations (Fig. 11) when the first narrow instability band plays an important role.…”

Section: Duration To Radiation Dominationsupporting

confidence: 79%

“…For M ∼ m Pl , ΔN rad is given by Eqs. (11) and (14). Note that with δ ≈ 0.126 → 0.1, ΔN br → ΔN rad .…”

Section: Observational Implications For Inflationary Observablesmentioning

confidence: 97%

mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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Self-resonance after inflation: Oscillons, transients, and radiation domination

2018

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C${\cal C}$osmological G${\cal G}$eometric P${\cal P}$hase F${\cal F}$rom P${\cal P}$ure Q${\cal Q}$uantum S${\cal S}$tates: A Study without/ with having Bell's Inequality Violation

Choudhury

2022

Fortschritte der Physik

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In this paper, using the concept of Lewis Riesenfeld invariant quantum operator method for finding continuous eigenvalues of quantum mechanical wave functions we derive the analytical expressions for the cosmological geometric phase, which is commonly identified to be the Pancharatnam Berry phase from primordial cosmological perturbation scenario. We compute this cosmological geometric phase from two possible physical situations, (1) In the absence of Bell's inequality violation and (2) In the presence of Bell's inequality violation having the contributions in the sub Hubble region (−kτ≫1$-k\tau \gg 1$), super Hubble region (−kτ≪1$-k\tau \ll 1$) and at the horizon crossing point (−kτ=1$-k\tau = 1$) for massless field (m/scriptH≪1$m/{\cal H}\ll 1$), partially massless field (m/scriptH∼1$m/{\cal H}\sim 1$) and massive/heavy field (m/scriptH≫1$m/{\cal H}\gg 1$), in the background of quantum field theory of spatially flat quasi De Sitter geometry. The prime motivation for this work is to investigate the various unknown quantum mechanical features of primordial universe. To give the realistic interpretation of the derived theoretical results we express everything initially in terms of slowly varying conformal time dependent parameters, and then to connect with cosmological observation we further express the results in terms of cosmological observables, which are spectral index/tilt of scalar mode power spectrum (nζ$n_{\zeta }$) and tensor‐to‐scalar ratio (r). Finally, this identification helps us to provide the stringent numerical constraints on the Pancharatnam Berry phase, which confronts well with recent cosmological observation.

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Causality Constraint on Circuit Complexity from COSMOEFT

Choudhury

Mukherjee

Pandey

et al. 2023

Fortschritte der Physik

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In this article, we investigate the physical implications of the causality constraint via the effective speed of sound cs(≤1)$c_s(\le 1)$ on Quantum Circuit Complexity (QCC) in the framework of Cosmological Effective Field Theory (COSMOEFT) using the two‐mode squeezed quantum states. This COSMOEFT setup is constructed using the Stnormalü$\ddot{\text{u}}$ckelberg trick with the help of the lowest dimensional operators, which are broken under time diffeomorphism. In this setup, we consider only the contributions from the two derivative terms in the background quasi‐de Sitter metric. Next, we compute the relevant measures of the circuit complexity and their cosmological evolution for different values of cs$c_s$ by following two different approaches, the Nielsen's approach and the Covariance matrix approach. Using this setup, we also compute the Von‐Neumann and the Rényi entropy, which finally establishes an underlying relationship between the entanglement entropy and the circuit complexity. Considering the scale factor and cs$c_s$ as parameters, our analysis of the circuit complexity measures and the entanglement entropy suggests several interesting unexplored features within the window, 0.024≤cs≤1$0.024\le c_s\le 1$, which is supported by both causality and cosmological observation. Finally, we comment on the connection between the circuit complexity, the entanglement entropy and the equilibrium temperature for different cs$c_s$ values lying within the mentioned window.

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Toward an effective field theory approach to reheating

Cited by 20 publications

References 82 publications

Self-resonance after inflation: Oscillons, transients, and radiation domination

Self-resonance after inflation: Oscillons, transients, and radiation domination

C${\cal C}$osmological G${\cal G}$eometric P${\cal P}$hase F${\cal F}$rom P${\cal P}$ure Q${\cal Q}$uantum S${\cal S}$tates: A Study without/ with having Bell's Inequality Violation

Causality Constraint on Circuit Complexity from COSMOEFT

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