Dark matter and baryon-number generation in quintessential inflation via hierarchical right-handed neutrinos

Hashiba, Soichiro; Yokoyama, Jun′ichi

doi:10.1016/j.physletb.2019.135024

Cited by 23 publications

(10 citation statements)

References 35 publications

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“…In the context of dark matter, the gravitational production of spin-0 particles was studied by refs. [29][30][31][32][33][34][35][36][37][38], spin-1/2 particles by refs. [39][40][41], spin-1 particles by refs.…”

Section: Introductionmentioning

confidence: 99%

Completely dark photons from gravitational particle production during the inflationary era

Kolb

Long

2021

J. High Energ. Phys.

106

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Starting with the de Broglie-Proca Lagrangian for a massive vector field, we calculate the number density of particles resulting from gravitational particle production (GPP) during inflation, with detailed consideration to the evolution of the number density through the reheating. We find plausible scenarios for the production of dark-photon dark matter of mass in a wide range, as low as a micro-electron volt to 1014 GeV. Gravitational particle production does not depend on any coupling of the dark photon to standard-model particles.

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Section: Introductionmentioning

confidence: 99%

Completely dark photons from gravitational particle production during the inflationary era

Kolb

Long

2021

J. High Energ. Phys.

106

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“…The subject of gravitational particle production has been studied extensively [43][44][45][46][47][48], and in the context of the inflaton field's quantum fluctuations, these are the seeds of structure that we observe on cosmological scales today. In the context of a spectator field, whose energy density is subdominant to the inflaton's during inflation, the phenomenon of gravitational particle production has important implications for the creation of superheavy particles, m χ ∼ H inf , including a variety of dark matter candidates [8,41,42,[49][50][51][52][53][54][55][56][57][58][59][60][61][62][63][64]. In this section, we briefly review how one calculates the relic density of particles that results from gravitational particle production.…”

Section: Gravitational Particle Productionmentioning

confidence: 99%

Superheavy scalar dark matter from gravitational particle production in $α$-attractor models of inflation

Ling,

Long

2021

Preprint

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We study the phenomenon of gravitational particle production as applied to a scalar spectator field in the context of α-attractor inflation. Assuming that the scalar has a minimal coupling to gravity, we calculate the abundance of gravitationally-produced particles as a function of the spectator's mass m χ and the inflaton's α parameter. If the spectator is stable and sufficiently weakly coupled, such that it does not thermalize after reheating, then a population of spin-0 particles is predicted to survive in the universe today, providing a candidate for dark matter. Inhomogeneities in the spatial distribution of dark matter correspond to an isocurvature component, which can be probed by measurements of the cosmic microwave background anisotropies. We calculate the dark matter-photon isocurvature power spectrum and by comparing with upper limits from Planck, we infer constraints on m χ and α. If the scalar spectator makes up all of the dark matter today, then for α = 10 and T rh = 10 4 GeV we obtain m χ > 1.8 × 10 13 GeV ≈ 1.2 m φ , where m φ is the inflaton's mass.

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“…While Eqs. ( 32) and (33) show the approximate parameter dependence of the energy densities of the gauge fields analytically, we need to perform the numerical integration to shown. We numerically evaluate the energy density of the electric and magnetic field in Eqs.…”

Section: A Gauge Field Amplificationmentioning

confidence: 99%

“…The latter is constrained by the number of relativistic degrees of freedom at the Big Bang Nucleosynthesis (BBN) [21] and at the recombination with the observation of the cosmic microwave background (CMB) [22]. Although there are intensive studies to address this issue and to find successful scenarios in the gravitational reheating [23][24][25][26][27][28][29][30][31][32][33][34][35], it is important to explore other possibilities of reheating in the inflationary models with kination.…”

Section: Introductionmentioning

confidence: 99%

Gauge Field Production and Schwinger Reheating in Runaway Axion Inflation

Hashiba,

Kamada,

Nakatsuka

2021

Preprint

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In a class of (pseudoscalar) inflation, inflationary phase is followed by a kination phase, where the Universe is dominated by the kinetic energy of the inflaton that runs away in a vanishing scalar potential. In this class of postinflationary evolution of the Universe, reheating of the Universe cannot be achieved by the inflaton particle decay, which requires its coherent oscillation in a quadratic potential. In this study, we explore the U(1) gauge field production through the Chern-Simons coupling between the pseudoscalar inflaton and the gauge field during the kination era and examine the subsequent pair-particle production induced by the amplified gauge field known as the Schwinger effect, which can lead to reheating of the Universe. We find that with a rough estimate of the Schwinger effect for the Standard Model hyper U(1) gauge field and subsequent thermalization of the pair-produced particles, a successful reheating of the Universe can be achieved by their eventual domination over the kinetic energy of the inflaton, with some reasonable parameter sets. This can be understood as a concrete realization of the "Schwinger reheating". Constraints from the later-time cosmology are also discussed.

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Dark matter and baryon-number generation in quintessential inflation via hierarchical right-handed neutrinos

Cited by 23 publications

References 35 publications

Completely dark photons from gravitational particle production during the inflationary era

Completely dark photons from gravitational particle production during the inflationary era

Superheavy scalar dark matter from gravitational particle production in $α$-attractor models of inflation

Gauge Field Production and Schwinger Reheating in Runaway Axion Inflation

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