Neutrino models of dark energy

Peccei, R.D.

doi:10.1103/physrevd.71.023527

Cited by 171 publications

(191 citation statements)

References 14 publications

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“…These behaviors of w are similar in three cases. The value of w turns to positive around z = 10, which is somewhat different from the result by Peccei [4], in which the power-law potential was also taken in the one family model and then, w becomes positive near z = 20.…”

Section: Evolutions Of Neutrino Masses and Wcontrasting

confidence: 49%

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Embedding the texture of the neutrino mass matrix into the MaVaNs scenario

Honda¹,

Takahashi²,

Tanimoto³

2006

J. High Energy Phys.

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We have embedded the texture of the neutrino mass matrix with three families into the MaVaNs scenario. We take the power-law potential of the acceleron field and a typical texture of active neutrinos, which is derived by the D 4 symmetry and predicts the maximal mixing of the atmospheric neutrino and the vanishing U e3 . Three cases of couplings among the dark fermion and active neutrinos are examined with the current cosmological data and the terrestrial neutrino experimental data. It is found that the neutrino flavor mixings evolve as well as the neutrino masses. Especially, U e3 develops into the non-vanishing one and θ atm deviates from the maximal mixing due to couplings among the dark fermion and active neutrinos. *

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Section: Evolutions Of Neutrino Masses and Wcontrasting

confidence: 49%

“…For our purpose it suffices to consider the neutrino mass as a function of the cosmic temperature T [4]. Since one can write down generally…”

Section: Dark Energy and Three Active Neutrino Massesmentioning

confidence: 99%

Embedding the texture of the neutrino mass matrix into the MaVaNs scenario

Honda¹,

Takahashi²,

Tanimoto³

2006

J. High Energy Phys.

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“…With this parameterization the mass of the second family is close to a linear regime for the baryonic densities present at Earth, and for the crust density of ρ ∼ 3 g/cm 3 we obtain ∆m 2 21 = 7.9 × 10 5 eV 2 , with a ρ 2 dependence. For the atmospheric neutrino scale, the third mass eigenvalue is already saturated for the Earth crust density, leading to ∆m 2 32 = 2.4×10 3 eV 2 .…”

Section: Reactor and Accelerator Neutrinosmentioning

confidence: 97%

“…The cosmological consequences of such coupling were widely addressed in a number of papers [2,3,4,5,6,7,8,9,10,11,12,13,14,15,16,17,18].…”

Section: Introductionmentioning

confidence: 99%

Possible scenario for MaVaN's as the only neutrino flavor conversion mechanism in the Sun

Holanda

2009

J. Cosmol. Astropart. Phys.

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Mass Varying neutrino mechanisms were proposed to link the neutrino mass scale with dark energy, addressing the coincidence problem. In some scenarios this mass can present a dependence on the baryonic density felt by neutrinos, creating an effective neutrino mass that depends both on the neutrino and baryonic densities. In this article we investigate the possibility that a neutrino effective mass is the only flavour conversion mechanism acting in neutrino oscillation experiments.We present a parameterization on the environmental effects on neutrino mass that produces the right flavour conversion probabilities for solar and terrestrial neutrinos experiments. * Electronic address: holanda@ifi.unicamp.br

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“…In turn, the latter is comparable (within the order of magnitude), to the energy density of cosmological neutrinos [1,2] [38]. (For more on the coincidence, see, e.g.…”

Section: Introductionmentioning

confidence: 99%

Mass varying neutrinos, quintessence, and the accelerating expansion of the Universe

2011

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We analyze the Mass Varying Neutrino (MaVaN) scenario. We consider a minimal model of massless Dirac fermions coupled to a scalar field, mainly in the framework of finite temperature quantum field theory. We demonstrate that the mass equation we find has non-trivial solutions only for special classes of potentials, and only within certain temperature intervals. We give most of our results for the Ratra-Peebles Dark Energy (DE) potential. The thermal (temporal) evolution of the model is analyzed. Following the time arrow, the stable, metastable and unstable phases are predicted. The model predicts that the present Universe is below its critical temperature and accelerates. At the critical point the Universe undergoes a firstorder phase transition from the (meta)stable oscillatory regime to the unstable rolling regime of the DE field. This conclusion agrees with the original idea of quintessence as a force making the Universe roll towards its true vacuum with zero Λ-term. The present MaVaN scenario is free from the coincidence problem, since both the DE density and the neutrino mass are determined by the scale M of the potential.Choosing M ∼ 10 −3 eV to match the present DE density, we can obtain the present neutrino mass in the range m ∼ 10 −2 − 1 eV and consistent estimates for other parameters of the Universe.

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Neutrino models of dark energy

Cited by 171 publications

References 14 publications

Embedding the texture of the neutrino mass matrix into the MaVaNs scenario

Embedding the texture of the neutrino mass matrix into the MaVaNs scenario

Possible scenario for MaVaN's as the only neutrino flavor conversion mechanism in the Sun

Mass varying neutrinos, quintessence, and the accelerating expansion of the Universe

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