Quintessential Kination and Thermal Production of SUSY e-WIMPs

Gómez, M. E.; Lola, S.; Pallis, C.; Rodríguez‐Quintero, J.

doi:10.1063/1.3131490

Cited by 5 publications

(3 citation statements)

References 16 publications

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“…Thermal production of WIMPs in the KS has been discussed in Refs. [68,[72][73][74][75][76], and has recently been investigated in Ref. [77], in light of recent data.…”

Section: Introductionmentioning

confidence: 99%

(Non-)Thermal Production of WIMPs during Kination

Visinelli

2018

Symmetry

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Understanding the nature of the Dark Matter (DM) is one of the current challenges in modern astrophysics and cosmology. Knowing the properties of the DM particle would shed light on physics beyond the Standard Model and even provide us with details of the early Universe. In fact, the detection of such a relic would bring us information from the pre-Big Bang Nucleosynthesis (BBN) period, an epoch from which we have no direct data, and could even hint at inflation physics. In this work, we assume that the expansion rate of the Universe after inflation is governed by the kinetic energy of a scalar field φ, in the so-called "kination" model. Adding to previous work on the subject, we assume that the φ field decays into both radiation and DM particles, which we take to be Weakly Interacting Massive Particles (WIMPs). The present abundance of WIMPs is then fixed during the kination period through either a thermal "freeze-out" or "freeze-in" mechanism, or through a non-thermal process governed by the decay of φ. We explore the parameter space of this theory with the requirement that the present WIMP abundance provides the correct relic budget. Requiring that BBN occurs during the standard cosmological scenario sets a limit on the temperature at which the kination period ends. Using this limit and assuming the WIMP has a mass mχ = 100 GeV, we obtain that the thermally-averaged WIMP annihilation cross section has to satisfy the constraints 4 × 10 −16 GeV −2 σv 2 × 10 −5 GeV −2 in order for having at least one of the production mechanism to yield the observed amount of DM. This result shows how the properties of the WIMP particle, if ever measured, can yield information on the pre-BBN content of the Universe.

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“…Thermal production of WIMPs in the KS has been discussed in Refs. [68,[72][73][74][75][76], and has recently been investigated in Ref. [77], in light of recent data.…”

Section: Introductionmentioning

confidence: 99%

(Non-)Thermal Production of WIMPs during Kination

Visinelli

2018

Symmetry

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show abstract

“…Thermal production of WIMPs in the KS has been discussed in Refs. [65,[69][70][71][72][73], and has recently been investigated in Ref. [74], in light of recent data.…”

Section: Introductionmentioning

confidence: 99%

(Non-)Thermal Production of WIMPs during Kination

Visinelli¹

2018

Preprint

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Understanding the nature of the Dark Matter (DM) is one of the current challenges in modern astrophysics and cosmology. Knowing the properties of the DM particle would shed light on physics beyond the Standard Model and even provide us with details of the early Universe. In fact, the detection of such a relic would bring us information from the pre-Big Bang Nucleosynthesis (BBN) period, an epoch from which we have no data, and could even hint at inflationary physics. In this work, we assume that the expansion rate of the Universe after inflationary is governed by the kinetic energy of a scalar field ϕ, in the so-called “kination” model. We assume that the ϕ field decays into both radiation and DM particles, which we take to be Weakly Interacting Massive Particles (WIMPs). The present abundance of WIMPs is then fixed during the kination period through either a thermal “freeze-out” or “freeze-in” mechanism, or through a non-thermal process governed by the decay of ϕ. We explore the parameter space of this theory with the requirement that the present WIMP abundance provides the correct DM relic budget. Requiring that BBN occurs during the standard cosmological scenario sets a limit on the temperature at which the kination period ends. Using this limit and assuming the WIMP has a mass mχ = 100 GeV, we obtain that the thermally-averaged WIMP annihilation cross section has to satisfy the constraints 3.5 × 10−16 GeV−2 ≲ (σv) ≲ 1.4 × 10−5 GeV−2 in order for having at least one of the production mechanism to yield the observed amount of DM. This result shows how the properties of the WIMP particle, if ever measured, can yield information on the pre-BBN content of the Universe.

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“…The thermal production of a weakly interacting massive particle during kination has been discussed in Refs. [134][135][136][137][138][139][140][141][142][143][144][145]. Since the kination field φ does not decay but it redshifts away, we assure entropy conservation by setting α = 1, while β = 1/3.…”

Section: • Kination Dominationmentioning

confidence: 99%

Axion miniclusters in modified cosmological histories

Visinelli

Redondo

2020

Phys. Rev. D

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If the symmetry breaking leading to the origin of the axion dark matter field occurs after the end of inflation and is never restored, then overdensities in the axion field collapse to form dense objects known in the literature as axion miniclusters. The estimates of the typical minicluster mass and radius strongly depend on the details of the cosmology at which the onset of axion oscillations begin. In this work we study the properties and phenomenology of miniclusters in alternative cosmological histories and find that they can change by many orders of magnitude. Our findings have direct implications on current and future experimental searches and, in the case of discovery, could be used to learn something about the Universe expansion prior to Big-Bang-Nucleosynthesys. * Electronic address: luca.visinelli@physics.uu.se † Electronic address: jredondo@unizar.es

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Quintessential Kination and Thermal Production of SUSY e-WIMPs

Cited by 5 publications

References 16 publications

(Non-)Thermal Production of WIMPs during Kination

(Non-)Thermal Production of WIMPs during Kination

(Non-)Thermal Production of WIMPs during Kination

Axion miniclusters in modified cosmological histories

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