Reheating in a brane monodromy inflation model

Abstract

We study reheating in a recently proposed brane "monodromy inflation" model in which the inflaton is the position of a D4 brane on a "twisted torus". Specifically, we study the repeated collisions between the D4 brane and a D6 brane (on which the Standard Model fields are assumed to be localized) at a fixed position along the monodromy direction as the D4 brane rolls down its potential. We find that there is no trapping of the rolling D4 brane until it reaches the bottom of its potential, and that reheating is entirely described by the last brane encounter. Previous collisions have negligible effect on the brane velocity and hence on the reheat temperature. In the context of our setup, reheating is efficient and the reheat temperature is therefore high.

Beauty is more attractive: particle production andmoduli trapping with higher dimensional interaction

“…Note that the Hamiltonian gives 22) JHEP01 (2014)141 where H is the VEV of the Hamiltonian H. Here, we can see that trapping force is weak near the ESP, but it becomes stronger when φ is away from the ESP. Except for a low-velocity limit (v ≪ gΛ 2 ), trapping force is significant when φ approaches φ ∼ Λ.…”

“…The potential V 0 = (ξ 2 − Z) 2 is too steep to satisfy the slow roll condition for sufficient N value in usual way. There are many inflationary models in which trapping plays a crucial role [20][21][22][23][24] and also the many-field model may accommodate slowroll inflation on the steep potential [3,25], but it is unclear if the GUT theory could be responsible for inflation [26]. We expect that inflaton becomes sufficiently slow because of particle production.…”

Inflation and String Theory

“…Reheating in a string theory model with a shift-symmetric inflaton poses particular difficulties, as explored in [557,560,562,564]. The general issue is that the shift symmetry that protects the inflaton simultaneously limits the couplings of the inflaton to the visible sector.…”

Global embedding of fibre inflation models

“…The 10D type IIB action for bulk fields receives α corrections which start contributing at O(α 3 ) and are encoded in several eight-derivative operators: 10) where the dots indicate the presence of subleading corrections for bulk fields, as well as additional terms related to local sources. S 3 denotes a set of eight-derivative operators which can be schematically written as:…”

“…This is crucial to have full control over the inflationary dynamics since it determines the properties of all directions orthogonal to the inflaton and fixes all the mass and energy scales in the model. On top of moduli stabilisation, other important issues to trust inflationary models building are the study of the post-inflationary cosmological history starting with reheating [9][10][11][12][13] and the interplay between inflation and other phenomenological implications of the same model like the supersymmetry breaking scale [14][15][16][17][18], the nature of dark matter [19][20][21][22][23] and dark radiation [24][25][26][27] or the origin of the matter-antimatter asymmetry [28,29].…”