Cosmology of mass-varying neutrinos driven by quintessence: Theory and observations

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

doi:10.1103/physrevd.73.083515

Cited by 168 publications

(157 citation statements)

References 80 publications

Supporting

Mentioning

150

Contrasting

Order By: Relevance

“…This is in fact the case most commonly studied in cosmology (for models with DE coupled to neutrinos, see Refs. [23,24]). One notes that the term γ χ (φ)L (χ) in the action Eq.…”

Section: Equations a Field Equations And Bianchi Identitiesmentioning

confidence: 99%

Growth of perturbations in dark matter coupled with quintessence

2005

View full text Add to dashboard Cite

We consider the evolution of linear perturbations in models with a nonminimal coupling between dark matter and scalar field dark energy. Growth of matter inhomogeneities in two examples of such models proposed in the literature are investigated in detail. Both of these models are based on a low-energy limit of effective string theory action, and have been previously shown to naturally lead to late acceleration of the universe. However, we find that these models can be ruled out by taking properly into account the impact of the scalar field coupling on the formation of structure in the dark matter density. In particular, when the transition to acceleration in these models begins, the interaction with dark energy enchances the small scale clustering in dark matter much too strongly. We discuss also the role of an effective small scale sound speed squared and the issue of adiabatic initial conditions in models with a coupled dark sector.

show abstract

“…This is in fact the case most commonly studied in cosmology (for models with DE coupled to neutrinos, see Refs. [23,24]). One notes that the term γ χ (φ)L (χ) in the action Eq.…”

Section: Equations a Field Equations And Bianchi Identitiesmentioning

confidence: 99%

Growth of perturbations in dark matter coupled with quintessence

2005

View full text Add to dashboard Cite

show abstract

“…The leptogenesis [9,10], the cosmo MSW effect of neutrinos [11] and the solar neutrino [12,13] have been studied in the context of this scenario. Cosmological discussions of the scenario are also presented [14,15,16,17,18,19].…”

Section: Introductionmentioning

confidence: 99%

Speed of sound in the mass varying neutrinos scenario

Takahashi

Tanimoto

2006

J. High Energy Phys.

View full text Add to dashboard Cite

We discuss about the speed of sound squared in the Mass Varying Neutrinos scenario (MaVaNs). Recently, it was argued that the MaVaNs has a catastrophic instability which is the emergence of an imaginary speed of sound at the non-relativistic limit of neutrinos.As the result of this instability, the neutrino-acceleron fluid cannot act as the dark energy.However, it is found that the speed of sound squared in the neutrino-acceleron fluid could be positive in our model. We examine the speed of sound in two cases of the scalar potential.One is the small fractional power-law potential and another is the logarithmic one. The power-law potential model with the right-handed neutrinos gives a stable one. † e-mail: takahasi@muse.sc.niigata-u.ac.jp ‡ e-mail: tanimoto@muse.sc.niigata-u.ac.jp I INTRODUCTIONOne of the most challenging questions in both cosmological and particle physics is the nature of the dark energy in the Universe. At the present epoch, the energy density of the Universe is dominated by a dark energy component, whose negative pressure causes the expansion of the Universe to accelerate. In order to clarify the origin of the dark energy, one has tried to understand the connection of the dark energy with particle physics. MaVaNs scenario leads to interesting phenomenological results. The neutrino oscillations may be a probe of the dark energy [6,7,8]. The leptogenesis [9,10], the cosmo MSW effect of neutrinos [11] and the solar neutrino [12,13] have been studied in the context of this scenario. Cosmological discussions of the scenario are also presented [14,15,16,17,18,19].The extension to the supersymmetry have been presented in ref. [20,21]. This scenario is also discussed in the context of the texture of the neutrino mass matrix with three families [22].Despite many implications of this scenario, ref. [23] showed that this scenario contains a catastrophic instability which occurs when neutrinos become non-relativistic. As neutrinos become non-relativistic, the speed of sound squared in the neutrino-acceleron fluid turns to be negative. As the result of this instability, neutrinos condense into neutrino nuggets, and 2 thus cannot act as the dark energy. However, we have found that the speed of sound squared in this fluid could be positive even though neutrinos are not enough relativistic. In order to realize the positive speed of sound squared, a constraint for the scalar potential is required.The paper is organized as follows: in Sec.II, we summarize the MaVaNs scenario with three families. Sec.III presents discussions for the speed of sound in the hydrodynamic picture. Sec.IV presents a stable model in the MaVaNs scenario. Sec.V devotes to the summary.

show abstract

“…Our work implies that CMB anisotropies as well as large scale structures will be able to constrain parameters of the theory tightly. In future we will investigate other potentials and couplings, elaborate on the degeneracies between the parameters and will use current data to constrain such models [10].…”

mentioning

confidence: 99%

“…In order to study the evolution of cosmological perturbations, we have extended the Boltzmann treatment of [12] to include the coupling between neutrinos and dark energy [10] (see e.g. [13] for detailed discussions on the physics of CMB anisotropies).…”

mentioning

confidence: 99%

Cosmology with Massive Neutrinos Coupled to Dark Energy

et al. 2006

Self Cite

View full text Add to dashboard Cite

Cosmological consequences of a coupling between massive neutrinos and dark energy are investigated. In such models, the neutrino mass is a function of a scalar field, which plays the role of dark energy. The evolution of the background and cosmological perturbations are discussed. We find that mass-varying neutrinos can leave a significant imprint on the anisotropies in the CMB and even lead to a reduction of power on large angular scales.

show abstract

Cosmology of mass-varying neutrinos driven by quintessence: Theory and observations

Cited by 168 publications

References 80 publications

Growth of perturbations in dark matter coupled with quintessence

Growth of perturbations in dark matter coupled with quintessence

Speed of sound in the mass varying neutrinos scenario

Cosmology with Massive Neutrinos Coupled to Dark Energy

Contact Info

Product

Resources

About