UltraViolet freeze-in

Elahi, Fatemeh; Kolda, Christopher; Unwin, James

doi:10.1007/jhep03(2015)048

Cited by 211 publications

(222 citation statements)

References 49 publications

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“…but remains out-of-equilibrium itself, and finally comprises the observed dark matter abundance, produced by particle decaysà la freeze-in mechanism [11][12][13][14][15][16][17][18][19][20]. As the Z 2 symmetric scalar field serves as both the inflaton and a FIMP ('Feebly Interacting Massive Particle') dark matter candidate, we name our scenario as the 'fimplaton' model.…”

Section: Jhep09(2016)049mentioning

confidence: 99%

Feebly interacting dark matter particle as the inflaton

Tenkanen

2016

J. High Energ. Phys.

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We present a scenario where a Z 2 -symmetric scalar field φ first drives cosmic inflation, then reheats the Universe but remains out-of-equilibrium itself, and finally comprises the observed dark matter abundance, produced by particle decaysà la freeze-in mechanism. We work model-independently without specifying the interactions of the scalar field besides its self-interaction coupling, λφ 4 , non-minimal coupling to gravity, ξφ 2 R, and coupling to another scalar field, gφ 2 σ 2 . We find the scalar field φ serves both as the inflaton and a dark matter candidate if 10 −9 λ g 10 −7 and 3 keV m φ 85 MeV for ξ = O(1). Such a small value of the non-minimal coupling is also found to be of the right magnitude to produce the observed curvature perturbation amplitude within the scenario. We also discuss how the model may be distinguished from other inflationary models of the same type by the next generation CMB satellites.

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Section: Jhep09(2016)049mentioning

confidence: 99%

Feebly interacting dark matter particle as the inflaton

Tenkanen

2016

J. High Energ. Phys.

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“…25,70 This component is generally ignored in most discussions of sterile neutrino dark matter from freeze-in, as only renormalizable interactions are considered. However, given that higher dimensional operators provide a natural framework for realizing extremely small couplings, which are necessary for the realization of (IR) freeze-in, it is always prudent to consider the possibility of a UV freeze-in component (see Ref.…”

Section: Uv Freeze-inmentioning

confidence: 99%

Sterile neutrino dark matter from freeze-in

Shakya

2016

Mod. Phys. Lett. A

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A sterile neutrino is a well-motivated and widely studied dark matter candidate. The most straightforward realization of sterile neutrino dark matter, through the DodelsonWidrow mechanism, is now ruled out by a combination of X-ray and Lyman-α measurements. An alternative production mechanism that is becoming increasingly popular in the literature is the freeze-in mechanism, involving frameworks where a feeble coupling to a particle -usually a scalar beyond the Standard Model -in the thermal bath results in a gradual accumulation of the sterile neutrino dark matter abundance. This article reviews the various motivations for realizing such frameworks in the literature, their common characteristic features, and phenomenological signatures.

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“…In models of freeze-in dark matter [11,[32][33][34][35][36][37][38], prior to freeze-in the abundance of DM is assumed negligible and the DM is generated by a portal operator connecting the hidden and visible sectors. The final relic abundance is controlled only by the DM mass and the portal operator if this is renormalisable (otherwise production is UV sensitive and may depend on the SM reheat temperature).…”

Section: Initial Conditions For Freeze-in Dark Mattermentioning

confidence: 99%

Symmetric and asymmetric reheating

Hardy¹,

Unwin²

2017

J. High Energ. Phys.

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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.

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UltraViolet freeze-in

Cited by 211 publications

References 49 publications

Feebly interacting dark matter particle as the inflaton

Feebly interacting dark matter particle as the inflaton

Sterile neutrino dark matter from freeze-in

Symmetric and asymmetric reheating

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