Suppression of parametric resonance and the viability of tachyonic preheating after multifield inflation

Battefeld, Diana; Battefeld, Thorsten; Giblin, John T.

doi:10.1103/physrevd.79.123510

Cited by 25 publications

(47 citation statements)

References 113 publications

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“…have approximately the same energy as the inflaton [74], even with three-leg interactions or tachyonic instabilities. These scenarios then rely on additional mechanisms or interactions to deplete the remaining energy in the inflation.…”

Section: Discussionmentioning

confidence: 99%

Gauge field preheating at the end of inflation

2013

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Here we consider the possibility of preheating the Universe via the parametric amplification of a massless, Uð1Þ Abelian gauge field. We assume that the gauge field is coupled to the inflaton via a dilatonlike coupling, a conformal factor with one free parameter. We present the results of high-resolution threedimensional simulations of this model and show that this mechanism efficiently preheats the Universe to a radiation-dominated final state.

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Section: Discussionmentioning

confidence: 99%

Gauge field preheating at the end of inflation

2013

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“…The parametric resonance for fluctuations δχ k will therefore be less efficient than in the models considered in Section 3. Indeed, if there are many inflaton fields, as in models like "Nflation", 147-150 then there is considerable reduction in the efficiency of preheating, related to the de-phasing of the pump fields ϕ I (t) 151,152 (however, see Refs. 153, 154).…”

Section: Multifield Inflationmentioning

confidence: 99%

Nonperturbative dynamics of reheating after inflation: A review

Amin

Hertzberg

Kaiser

et al. 2014

Int. J. Mod. Phys. D

444

498

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Our understanding of the state of the universe between the end of inflation and big bang nucleosynthesis (BBN) is incomplete. The dynamics at the end of inflation are rich and a potential source of observational signatures. Reheating, the energy transfer between the inflaton and Standard Model fields (possibly through intermediaries) and their subsequent thermalization, can provide clues to how inflation fits in with known high-energy physics. We provide an overview of our current understanding of the nonperturbative, nonlinear dynamics at the end of inflation, some salient features of realistic particle physics models of reheating, and how the universe reaches a thermal state before BBN. In addition, we review the analytical and numerical tools available in the literature to study preheating and reheating and discuss potential observational signatures from this fascinating era.

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“…For the most part, studies of preheating have focused on the existence and stability of these processes in the presence of different inflationary potentials, e.g., Refs. [17][18][19][20][21][22], multiple fields [23], and multiple decay channels [24]. DBI inflation might end with a coherently oscillating scalar field, and it has been unclear whether preheating can persist in the presence of nonlinear terms in its equation of motion.…”

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confidence: 99%

Preheating with Nonminimal Kinetic Terms

et al. 2013

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We present the first (3 + 1)-dimensional numerical simulations of scalar fields with nonminimal kinetic terms. As an example, we examine the existence and stability of preheating in the presence of a Dirac-Born-Infeld inflaton coupled to a canonical matter field. The simulations represent the full nonlinear theory in the presence of an expanding universe. We show that parametric resonance in the matter field along with self-resonance in the inflaton repopulate the universe with matter particles as efficiently as in traditional preheating.Scalar fields need not be Klein-Gordon-like in four dimensions; theories that include extra dimensions, whether large or small, have effective four-dimensional kinetic terms that are nonminimal. This has led to an increased interest in the dynamics of nonminimal models both to describe inflation, e.g. Dirac-Born-Infeld (DBI) inflation [1], and even more recently, dark energy [2][3][4]. In this Letter, we will focus on DBI inflation, as an example of a system for which we have a scalar degree of freedom whose behavior is self-consistent and stable and whose nonminimal behavior is central to the dynamics of the model. Here, we focus on what happens at the end of inflation when the scalar inflaton becomes inhomogeneous and its couplings to other fields are important. To our knowledge, these are the first three-dimensional lattice simulations of this type of field theory.Preheating [5][6][7][8][9][10][11][12][13][14][15][16][17] provides a mechanism by which the cold postinflationary universe can quickly and efficiently transfer energy into a matter sector, via a period of parametric resonance or a regime of tachyonic instability. For the most part, studies of preheating have focused on the existence and stability of these processes in the presence of different inflationary potentials, e.g., Refs. [17][18][19][20][21][22], multiple fields [23], and multiple decay channels [24]. DBI inflation might end with a coherently oscillating scalar field, and it has been unclear whether preheating can persist in the presence of nonlinear terms in its equation of motion. The search for preheating in nonminimal models began in the work of Ref. [25], where the authors showed that a canonical scalar field can enhance the effects of parametric resonance in a coupled nonminimal matter field.

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Suppression of parametric resonance and the viability of tachyonic preheating after multifield inflation

Cited by 25 publications

References 113 publications

Gauge field preheating at the end of inflation

Gauge field preheating at the end of inflation

Nonperturbative dynamics of reheating after inflation: A review

Preheating with Nonminimal Kinetic Terms

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