Visible sector inflation and the right thermal history in light of Planck data

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Explaining baryon asymmetry, dark matter and inflation are important elements of a successful theory that extends beyond the Standard Model of particle physics. In this paper we explore these issues within Next-to-Minimal Supersymmetric Standard Model (NMSSM) by studying the conditions for a strongly first order electroweak phase transition, the abundance of the lightest supersymmetric particle (LSP), and inflation driven by a gauge invariant flat direction of MSSM -made up of right handed squarks. We present the regions of parameter space which can yield successful predictions for cosmic microwave background (CMB) radiation through inflation, the observed relic density for dark matter, and successful baryogenesis. Constrains by collider measurements (such as the recent Higgs mass bound), branching ratios of rare, flavour violating decays, and the invisible Z decay width are also imposed. We explore where dark matter interactions with xenon nuclei would fall within current bounds of XENON100 and the projected limits for the XENON1T and LUX experiments.

Section: Gauge Invariant Inflatonmentioning

confidence: 64%

Baryogenesis, dark matter and inflation in the next-to-minimal supersymmetric standard model

Balázs

Mazumdar

Pukartas

et al. 2014

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“…This scenario has been discussed extensively, and has been extremely successful with the Planck data explaining the spectral tilt right on the observed central value, with Gaussian perturbations with the right amplitude [36,62].…”

Section: Jhep04(2014)077mentioning

confidence: 93%

Constraining $ \mathcal{N} $ = 1 supergravity inflationary framework with non-minimal Kähler operators

Choudhury

Mazumdar

Pukartas

2014

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In this paper we will illustrate how to constrain unavoidable Kähler corrections for N = 1 supergravity (SUGRA) inflation from the recent Planck data. We will show that the non-renormalizable Kähler operators will induce in general non-minimal kinetic term for the inflaton field, and two types of SUGRA corrections in the potential -the Hubbleinduced mass (c H ), and the Hubble-induced A-term (a H ) correction. The entire SUGRA inflationary framework can now be constrained from (i) the speed of sound, c s , and (ii) from the upper bound on the tensor to scalar ratio, r ⋆ . We will illustrate this by considering a heavy scalar degree of freedom at a scale, M s , and a light inflationary field which is responsible for a slow-roll inflation. We will compute the corrections to the kinetic term and the potential for the light field explicitly. As an example, we will consider a visible sector inflationary model of inflation where inflation occurs at the point of inflection, which can match the density perturbations for the cosmic microwave background radiation, and also explain why the universe is filled with the Standard Model degrees of freedom. We will scan the parameter space of the non-renormalizable Kähler operators, which we find them to be order O(1), consistent with physical arguments. While the scale of heavy physics is found to be bounded by the tensor-to scalar ratio, and the speed of sound, O 10 11 ≤ M s ≤ 10 16 GeV, for 0.02 ≤ c s ≤ 1 and 10 −22 ≤ r ⋆ ≤ 0.12.

“…This makes model building strong decays of χ i to only one sector straightforward. In contrast, attempting to make the inflaton part of the visible sector, in such a way that prevents it decaying to a generic hidden sector is more difficult [99].…”

Section: Jhep09(2017)113mentioning

confidence: 99%

Symmetric and asymmetric reheating

Hardy¹,

Unwin²

2017

We study models in which the inflaton is coupled to two otherwise decoupled sectors, and the effect of preheating and related processes on their energy densities during the evolution of the universe. Over most of parameter space, preheating is not disrupted by the presence of extra sectors, and even comparatively weakly coupled sectors can get an order 1 fraction of the total energy at this time. If two sectors are both preheated, the high number densities could also lead to inflaton mediated thermalisation. If only one sector is preheated, Bose enhancement of the late time inflaton decays may cause significant deviations from the perturbative prediction for their relative reheat temperatures. Meanwhile, in Non-Oscillatory inflation models resonant effects can result in exponentially large final temperature differences between sectors that have similar couplings to the inflaton. Asymmetric reheating is potentially relevant for a range of beyond the Standard Model physics scenarios. We show that in dark matter freeze-in models, hidden sector temperatures a factor of 10 below that of the visible sector are typically needed for the relic abundance to be set solely by freeze-in dynamics.