Erratum: Cosmology of mass-varying neutrinos driven by quintessence: Theory and observations [Phys. Rev. D<b>73</b>, 083515 (2006)]

Brookfield, Anthony W.; Bruck, Carsten van de; Mota, David F.; Tocchini-Valentini, Domenico

doi:10.1103/physrevd.76.049901

Cited by 72 publications

(104 citation statements)

References 35 publications

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“…In this case the evolution of the field is highly non-adiabatic [65,66]. However, this model has the disadvantage that the neutrino mass is no longer related naturally to the dark energy density and equation of state.…”

Section: Jcap01(2008)026mentioning

confidence: 99%

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Neutrino dark energy—revisiting the stability issue

Bjælde¹,

Brookfield²,

Bruck³

et al. 2008

J. Cosmol. Astropart. Phys.

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A coupling between a light scalar field and neutrinos has been widely discussed as a mechanism for linking (time varying) neutrino masses and the present energy density and equation of state of dark energy. However, it has been pointed out that the viability of this scenario in the non-relativistic neutrino regime is threatened by the strong growth of hydrodynamic perturbations associated with a negative adiabatic sound speed squared. In this paper we revisit the stability issue in the framework of linear perturbation theory in a model independent way. The criterion for the stability of a model is translated into a constraint on the scalar-neutrino coupling, which depends on the ratio of the energy densities in neutrinos and cold dark matter. We illustrate our results by providing meaningful examples both for stable and unstable models.

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Section: Jcap01(2008)026mentioning

confidence: 99%

“…[23,54,66,75,76] and references therein), we will simply state them here for neutrinos coupled to a scalar field.…”

Section: Evolution Of the Perturbationsmentioning

confidence: 99%

Neutrino dark energy—revisiting the stability issue

Bjælde¹,

Brookfield²,

Bruck³

et al. 2008

J. Cosmol. Astropart. Phys.

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“…The nature of both DM and DE being unknown, there is no physical argument to exclude their interaction. On the contrary, arguments in favor of such interaction have been suggested [17], and more recently they have been extended to include neutrinos [18]. As a result of the interaction, the matter density drops with the scale factor at of the Friedmann-RobertsonWalker metric more slowly than a ÿ3 .…”

Section: Introductionmentioning

confidence: 99%

Matter density perturbations in interacting quintessence models

2006

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Models with dark energy decaying into dark matter have been proposed to solve the coincidence problem in cosmology.We study the effect of such coupling in the matter power spectrum. Because of the interaction, the growth of matter density perturbations during the radiation dominated regime is slower compared to noninteracting models with the same ratio of dark matter to dark energy today. This effect introduces a damping on the power spectrum at small scales proportional to the strength of the interaction, c 2 , and similar to the effect generated by ultrarelativistic neutrinos. The interaction also shifts matterradiation equality to larger scales. We compare the matter power spectrum of interacting quintessence models with the measurments of the 2-degree field galaxy redshift survey (2dFGRS). The data are insensitive to values of c 2 ≤ 10 -3 but strongly constrain larger values. We particularize our study to models that during radiation domination have a constant dark matter to dark energy ratio. Models with dark energy decaying into dark matter have been proposed to solve the coincidence problem in cosmology. We study the effect of such coupling in the matter power spectrum. Because of the interaction, the growth of matter density perturbations during the radiation dominated regime is slower compared to noninteracting models with the same ratio of dark matter to dark energy today. This effect introduces a damping on the power spectrum at small scales proportional to the strength of the interaction, c 2 , and similar to the effect generated by ultrarelativistic neutrinos. The interaction also shifts matterradiation equality to larger scales. We compare the matter power spectrum of interacting quintessence models with the measurments of the 2-degree field galaxy redshift survey (2dFGRS). The data are insensitive to values of c 2 10 ÿ3 but strongly constrain larger values. We particularize our study to models that during radiation domination have a constant dark matter to dark energy ratio.

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“…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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Erratum: Cosmology of mass-varying neutrinos driven by quintessence: Theory and observations [Phys. Rev. D73, 083515 (2006)]

Cited by 72 publications

References 35 publications

Neutrino dark energy—revisiting the stability issue

Neutrino dark energy—revisiting the stability issue

Matter density perturbations in interacting quintessence models

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

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