Gravitational wave production from preheating with trilinear interactions

Cosme, Catarina; Figueroa, Daniel G.; Nicolas, Loayza,

doi:10.1088/1475-7516/2023/05/023

Cited by 15 publications

(4 citation statements)

References 145 publications

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“…Notably, even if λ ≪ 1, as required by the measured amplitude of the primordial curvature fluctuation, the growth of inhomogeneities can be amplified by the accumulation of the (bosonic) field fluctuations over the oscillation of the inflaton. This parametric self-resonance persists despite the expansion of the universe, leading then to the exponential growth of non-zero momentum modes until they backreact into the homogeneous condensate, fragmenting it [41][42][43][44][45][46][47][48][49][50][51][52][53][54][55]. The resulting inhomogeneous field distribution can become localized in transient structures, lasting for a few oscillations, or into long-lived, soliton-like structures called oscillons [41,42,47,[56][57][58].…”

Section: Jcap12(2023)028mentioning

confidence: 99%

Effects of fragmentation on post-inflationary reheating

Garcia,

Gross,

Mambrini

et al. 2023

J. Cosmol. Astropart. Phys.

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We consider the effects of fragmentation on the post-inflationary epoch of reheating. In simple single field models of inflation, an inflaton condensate undergoes an oscillatory phase once inflationary expansion ends. The equation of state of the condensate depends on the shape of the scalar potential, V(ϕ), about its minimum. Assuming V(ϕ) ∼ ϕk , the equation of state parameter is given by w = Pϕ /ρϕ = (k - 2)/(k + 2). The evolution of condensate and the reheating process depend on k. For k ≥ 4, inflaton self-interactions may lead to the fragmentation of the condensate and alter the reheating process. Indeed, these self-interactions lead to the production of a massless gas of inflaton particles as w relaxes to 1/3. If reheating occurs before fragmentation, the effects of fragmentation are harmless. We find, however, that the effects of fragmentation depend sensitively to the specific reheating process. Reheating through the decays to fermions is largely excluded since perturbative couplings would imply that fragmentation occurs before reheating and in fact could prevent reheating from completion. Reheating through the decays to boson is relatively unaffected by fragmentation and reheating through scatterings results in a lower reheating temperature.

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Section: Jcap12(2023)028mentioning

confidence: 99%

Effects of fragmentation on post-inflationary reheating

Garcia,

Gross,

Mambrini

et al. 2023

J. Cosmol. Astropart. Phys.

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“…As it has recently been shown in [82], the presence of inflaton self-interactions can lead to inflaton fragmentation that can severely influence the reheating dynamics. A complete analysis including all such collective effects requires a dedicated lattice simulation [82][83][84], which we plan to address in a future work.…”

Section: Bbn: T Rhmentioning

confidence: 99%

Measuring inflaton couplings via primordial gravitational waves

Barman

Ghoshal

Grza̧dkowski

et al. 2023

J. High Energ. Phys.

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We investigate the reach of future gravitational wave (GW) detectors in probing inflaton couplings with visible sector particles that can either be bosonic or fermionic in nature. Assuming reheating takes place through perturbative quantum production from vacuum in presence of classical inflaton background field, we find that the spectral energy density of the primordial GW generated during inflation becomes sensitive to inflaton-matter coupling. We conclude, obeying bounds from Big Bang Nucleosysthesis and Cosmic Microwave Background, that, e.g., inflaton-scalar couplings of the order of ~ 𝒪(10−20) GeV fall within the sensitivity range of several proposed GW detector facilities. However, this prediction is sensitive to the size of the inflationary scale, nature of the inflaton-matter interaction and shape of the potential during reheating. Having found the time-dependent effective inflaton decay width, we also discuss its implications for dark matter (DM) production from the thermal plasma via UV freeze-in during reheating. It is shown, that one can reproduce the observed DM abundance for its mass up to several PeVs, depending on the dimension of the operator connecting DM with the thermal bath and the associated scale of the UV physics. Thus we promote primordial GW to observables sensitive to feebly coupled inflaton, which is very challenging if not impossible to test in conventional particle physics laboratories or astrophysical measurements.

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“…[19]). Possible gravitational relics, such as gravitational waves [20][21][22][23][24][25][26][27][28], collapsed structures like JCAP03(2024)017 primordial black holes [14,[29][30][31][32][33][34][35], or compact mini halos [36,37], offer potential probes into the reheating epoch.…”

Section: Introductionmentioning

confidence: 99%

Gauge preheating with full general relativity

Adshead,

Giblin,

Grutkoski

et al. 2024

J. Cosmol. Astropart. Phys.

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We study gauge preheating following pseudoscalar-driven inflation in full general relativity. We implement the Baumgarte-Shapiro-Shibata-Nakamura (BSSN) scheme to solve the full nonlinear evolution of the metric alongside the dynamics of the pseudoscalar and gauge fields. The dynamics of the background and emission of gravitational waves are broadly consistent with simulations in a Friedmann-Lemaître-Robertson-Walker (FLRW) spacetime. We find large, localized overdensities in the BSSN simulations of order δ = δρ/ρ ∼ 30, and the dimensionless power spectrum of δ peaks above unity. These overdense regions are seeded on length scales only slightly smaller than the horizon, and have a compactness C ∼ 0.1. The scale of peak compactness is shorter than the Jeans length, which implies that pressure of the matter fields plays an important role in the evolution of these objects.

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Gravitational wave production from preheating with trilinear interactions

Cited by 15 publications

References 145 publications

Effects of fragmentation on post-inflationary reheating

Effects of fragmentation on post-inflationary reheating

Measuring inflaton couplings via primordial gravitational waves

Gauge preheating with full general relativity

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