Preheating after Multi-Field Inflation

Battefeld, Diana

doi:10.1016/j.nuclphysbps.2009.07.050

Cited by 13 publications

(19 citation statements)

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“…The interval for g is not particularly wide, but allowed values do not appear to be overly fine tuned either and cover the same range commonly considered for studies of preheating after inflation [104,123,124]. In fact, the fields at ESPs in the vicinity of the final resting place can act as preheat matter fields, as investigated in [106]: there, it was found that preheating is qualitatively different than in models that have an ESP at the VEV of the inflatons; while de-phasing of inflatons tends to suppress parametric resonance [116][117][118][119] (see [118,125,126] for the case of two inflations, that still permits resonances), two new effects leading to efficient preheating were found: particle production during the first in-fall can already comprise a seizable energy transfer if the trapped inflation regime lasts until preheating commences, but it is never complete. Subsequent broad resonance is generically suppressed due to de-phasing of the fields, but if an 8 Taking e.g.…”

Section: The Power-spectrum From Back-scatteringmentioning

confidence: 98%

“…As long as the potential is steep enough, the trajectory is traversed at this constant speed; thus, functional fine tuning, i.e., the η problem, is relaxed. Preheating was discussed in [106], entailing qualitatively new resonance effects: efficient preheating is likely for dense distributions, x 0.001, in contrast to preheating with a single ESP at the VEV of the inflatons [116][117][118][119].…”

Section: Introductionmentioning

confidence: 99%

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Particle production during inflation in light of Planck data

Battefeld¹,

Battefeld²,

Fiene³

et al. 2014

Phys. Rev. D

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We consider trapped inflation in a higher dimensional field space: particle production at a dense distribution of extra species points leads to a terminal velocity at which inflation can be driven in steep potentials. We compute an additional, nearly scale invariant contribution to the powerspectrum, caused by back-scattering of the continuously produced particles. Since this contribution has a blue tilt, it has to be sub-dominant, leading to an upper bound on the coupling constant between the inflatons and the extra species particles. The remaining allowed parameter space is narrow. 2 See [108] for particle production at a point of enhanced gauge symmetry after inflation within the MSSM [109-111]. 3 Monodromy inflation [95] is a realization of trapped inflation [84, 94]. 4 This terminal velocity at weak coupling should not be confused with the speed limit at strong coupling [114] leading to DBIinflation [115]. arXiv:1309.4082v2 [astro-ph.CO]

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Section: The Power-spectrum From Back-scatteringmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

Particle production during inflation in light of Planck data

Battefeld¹,

Battefeld²,

Fiene³

et al. 2014

Phys. Rev. D

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“…We wish to include several preheat "matter" fields that become light at different ESPs in the vicinity of | ϕ| = 0; we deliberately avoid putting an ESP at | ϕ| = 0, since preheating of such a field is well understood (see [8,9,15,38,[40][41][42]84] for a small, non-representative collection, with particular focus on multiple inflatons) and generally suppressed if N > few [15,[38][39][40].…”

Section: Matter Fieldsmentioning

confidence: 99%

“…An observable by-product of preheating can be gravitational waves [28][29][30][31][32][33][34][35][36][37]. The majority of these phenomenological studies focus on one (see the reviews [1,2]) or several [15,[38][39][40][41][42] inflaton fields, coupled to a single degree of freedom that becomes light at the vacuum expectation value (VEV) of the inflatons. For example, in standard, single-field chaotic inflation with potential V (ϕ) = m 2 ϕ 2 /2, one can introduce another light scalar field that couples to the inflaton via the interaction Lagrangian L = −g 2 χ 2 ϕ 2 /2, such that the effective mass of χ is minimal at the VEV ϕ = 0.…”

Section: Introductionmentioning

confidence: 99%

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Enhanced preheating after multi-field inflation: on the importance of being special

Battefeld¹,

Eggemeier²,

Giblin³

2012

J. Cosmol. Astropart. Phys.

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Abstract. We discuss preheating after multi-field inflation in the presence of several preheat matter fields that become light in the vicinity of (but not at) the inflatons' VEV, at distinct extra-species-points (ESP); this setup is motivated by inflationary models that include particle production during inflation, e.g. trapped inflation, grazing ESP encounters or modulated trapping, among others. While de-phasing of inflatons tends to suppress parametric resonance, we find two new effects leading to efficient preheating: particle production during the first in-fall (efficient if many preheat matter fields are present) and a subsequent (narrow) resonance phase (efficient if an ESP happens to be at one of several distinct distances from the inflatons' VEV). Particles produced during the first in-fall are comprised of many species with low occupation number, while the latter are made up of a few species with high occupation number.We provide analytic descriptions of both phases in the absence of back-reaction, which we test numerically. We further perform lattice simulations to investigate the effects of backreaction. We find resonances to be robust and the most likely cause of inflaton decay in multi-field trapped inflation if ESP distributions are dense.

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A terminal velocity on the landscape: particle production near extra species loci in higher dimensions

Battefeld

Battefeld²

2010

J. High Energ. Phys.

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We investigate particle production near extra species loci (ESL) in a higher dimensional field space and derive a speed limit in moduli space at weak coupling. This terminal velocity is set by the characteristic ESL-separation and the coupling of the extra degrees of freedom to the moduli, but it is independent of the moduli's potential if the dimensionality of the field space is considerably larger than the dimensionality of the loci, D ≫ d. Once the terminal velocity is approached, particles are produced at a plethora of nearby ESLs, preventing a further increase in speed via their backreaction. It is possible to drive inflation at the terminal velocity, providing a generalization of trapped inflation with attractive features: we find that more than sixty e-folds of inflation for sub-Planckian excursions in field space are possible if ESLs are ubiquitous, without fine tuning of initial conditions and less tuned potentials. We construct a simple, observationally viable model with a slightly red scalar power-spectrum and suppressed gravitational waves; we comment on the presence of additional observational signatures originating from IR-cascading and individual massive particles. We also show that moduli-trapping at an ESL is suppressed for D ≫ d, hindering dynamical selection of high-symmetry vacua on the landscape based on this mechanism.

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Preheating after Multi-Field Inflation

Cited by 13 publications

References 14 publications

Particle production during inflation in light of Planck data

Particle production during inflation in light of Planck data

Enhanced preheating after multi-field inflation: on the importance of being special

A terminal velocity on the landscape: particle production near extra species loci in higher dimensions

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