Oscillation effects on thermalization of the neutrinos in the universe with low reheating temperature

Ichikawa, Kazuhide; Kawasaki, Masahiro; Takahashi, Fuminobu

doi:10.1103/physrevd.72.043522

Cited by 202 publications

(213 citation statements)

References 66 publications

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“…This temperature needs to be larger than 2 MeV in order for standard BBN to happen [26]. The baryon asymmetry and the dark matter component of the universe also needs to be generated before BBN.…”

Section: Case (A): the S → Hh Decay Is Open (M S > 2m H )mentioning

confidence: 99%

Gauge mediation in supergravity and gravitino dark matter

Ibe

Kitano

2007

Phys. Rev. D

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Gravitinos and hidden sector fields often cause a cosmological disaster in supersymmetric models. We find that a model with gravitational gauge mediation solves such a problem quite naturally. The µ-problem is also absent in the model. Moreover, the abundance of gravitinos explains correct amount of dark matter of the universe. The dark matter abundance can be calculated without detailed information on the thermal history of the universe such as the reheating temperature after inflation.

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Section: Case (A): the S → Hh Decay Is Open (M S > 2m H )mentioning

confidence: 99%

Gauge mediation in supergravity and gravitino dark matter

Ibe

Kitano

2007

Phys. Rev. D

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“…(16) and (21) for all combinations of the variables m χ , T RH , and σv that produce the observed dark matter abundance of Ω χ h 2 = 0.12 [44]. We set the minimum allowed reheat temperature to 3 MeV to ensure that the period of kination does not alter the cosmic microwave background or the abundances of light elements [4][5][6][7][8]. 2 Next, we compare our allowed parameters to current constraints on m χ and σv from Fermi-LAT and H.E.S.S.…”

Section: Constraints On Kinationmentioning

confidence: 99%

“…The energy scale of inflation is not known, but it is generally assumed to be greater than 10 10 GeV. The successful BBN prediction of the abundances of light elements only requires that the Universe be radiation dominated at a temperature of 3 MeV [4][5][6][7][8]. Thus, there is a gap in the cosmological record between the theorized energy scale of inflation and 3 MeV.…”

Section: Introductionmentioning

confidence: 99%

New constraints on dark matter production during kination

Redmond

Erickcek

2017

Phys. Rev. D

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Our ignorance of the period between the end of inflation and the beginning of Big Bang Nucleosynthesis limits our understanding of the origins and evolution of dark matter. One possibility is that the Universe's energy density was dominated by a fast-rolling scalar field while the radiation bath was hot enough to thermally produce dark matter. We investigate the evolution of the dark matter density and derive analytic expressions for the dark matter relic abundance generated during such a period of kination. Kination scenarios in which dark matter does not reach thermal equilibrium require σv < 2.7 × 10 −38 cm 3 s −1 to generate the observed dark matter density while allowing the Universe to become radiation dominated by a temperature of 3 MeV. Kination scenarios in which dark matter does reach thermal equilibrium require σv > 3 × 10 −26 cm 3 s −1 in order to generate the observed dark matter abundance. We use observations of dwarf spheroidal galaxies by the Fermi Gamma-Ray Telescope and observations of the Galactic Center by the High Energy Stereoscopic System to constrain these kination scenarios. Combining the unitarity constraint on σv with these observational constraints sets a lower limit on the temperature at which the Universe can become radiation dominated following a period of kination if σv > 3 × 10 −31 cm 3 s −1 . This lower limit is between 0.05 GeV and 1 GeV, depending on the dark matter annihilation channel.

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“…After dominating the Universe, moduli decay to lighter particles in the minimal extension of supersymmetric standard model (MSSM). The moduli decay temperature can be higher than O(1) MeV for the moduli mass heavier than about 10 TeV if their interactions are suppressed by the Planck mass, thus avoiding bounds from the big bang nucleosynthesis (BBN) [17][18][19][20]. In this paper we study a baryogenesis scenario in which the baryon asymmetry is generated through CP violating decay of gluino into quark and squark, followed by baryon-number violating squark decay.…”

Section: Jhep02(2014)062mentioning

confidence: 99%

“…The saxion couplings to gluon and gluino are given (in two-component notation) by 20) where G µν is the gluon field strength and m s is the saxion mass, and the order unity constant κ is determined by how the saxion is stabilized. The above couplings mediate the saxion decay into a gluon pair and a gluino pair with…”

Section: Jhep02(2014)062mentioning

confidence: 99%

Moduli-induced baryogenesis

Ishiwata

Jeong

Takahashi

2014

J. High Energ. Phys.

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We study a scenario for baryogenesis in modular cosmology and discuss its implications for the moduli stabilization mechanism and the supersymmetry (SUSY) breaking scale. If moduli fields dominate the Universe and decay into the standard model particles through diatonic couplings, the right amount of baryon asymmetry can be generated through CP violating decay of gluino into quark and squark followed by baryon-number violating squark decay. We find that, in the KKLT-type moduli stabilization, at least two non-perturbative terms are required to obtain a sizable CP phase, and that the successful baryogenesis is possible for the soft SUSY breaking mass heavier than O(1) TeV. A part of the parameter space for successful baryogenesis can be probed at the collider experiments, dinucleon decay search experiment, and the measurements of electric dipole moments of neutron and electron. It is also shown that similar baryogenesis works in the case of the gravitino-or the saxion-dominated Universe.

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Oscillation effects on thermalization of the neutrinos in the universe with low reheating temperature

Cited by 202 publications

References 66 publications

Gauge mediation in supergravity and gravitino dark matter

Gauge mediation in supergravity and gravitino dark matter

New constraints on dark matter production during kination

Moduli-induced baryogenesis

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