Supersymmetric theories of neutrino dark energy

Fardon, Rob; Nelson, Ann E.; Weiner, Neal

doi:10.1088/1126-6708/2006/03/042

Cited by 69 publications

(129 citation statements)

References 58 publications

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“…Our work builds on previous analyses of MaVaN [15,17,22,23,24], chameleon [19,20], and general coupled scenarios [16]. Our numerical analyses of coupled CDM and MaVaN models reinforce our analytic findings.…”

Section: Discussionsupporting

confidence: 76%

“…The impact of adiabatic instabilities has been discussed extensively in the context of MaVaN models, in which the light mass of the neutrino and the recent accelerative era are twinned together through a scalar field coupling [22, 23,24]. The adiabatic instability was shown to be a concern in these models with the implication of forming compact localized regions of neutrinos after undergoing dramatic adiabatic collapse [15].…”

Section: Mass Varying Neutrino ("Mavan") Modelsmentioning

confidence: 99%

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Adiabatic instability in coupled dark energy/dark matter models

2008

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We consider theories in which there exists a nontrivial coupling between the dark matter sector and the sector responsible for the acceleration of the universe. Such theories can possess an adiabatic regime in which the quintessence field always sits at the minimum of its effective potential, which is set by the local dark matter density. We show that if the coupling strength is much larger than gravitational, then the adiabatic regime is always subject to an instability. The instability, which can also be thought of as a type of Jeans instability, is characterized by a negative sound speed squared of an effective coupled dark matter/dark energy fluid, and results in the exponential growth of small scale modes. We discuss the role of the instability in specific coupled CDM and Mass Varying Neutrino (MaVaN) models of dark energy, and clarify for these theories the regimes in which the instability can be evaded due to non-adiabaticity or weak coupling.

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Section: Discussionsupporting

confidence: 76%

Section: Mass Varying Neutrino ("Mavan") Modelsmentioning

confidence: 99%

Adiabatic instability in coupled dark energy/dark matter models

2008

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“…[20,21]. This scenario is also discussed in the context of the texture of the neutrino mass matrix with three families [22].…”

Section: Introductionmentioning

confidence: 99%

Speed of sound in the mass varying neutrinos scenario

Takahashi

Tanimoto

2006

J. High Energy Phys.

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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.

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“…Hinting at a possible connection between the two, this has understandably led to speculations that the physics of neutrinos and dark energy might be linked in various ways [18][19][20][72][73][74][75][76][77][78][79][80][81]. In MaVaN scenarios, the neutrino masses are tied to dark energy and evolve cosmologically [20,[82][83][84][85]. The present model, however, requires no time sensitivity of the physical constants.…”

Section: Dark Energy Decaymentioning

confidence: 92%

Planetary Heating by Neutrinos: Long-Term Habitats for Aquatic Life if Dark Energy Decays Favourably

Spivey¹

2013

JMP

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The potential cosmological and astrobiological implications of neutrinos are considered. Dark energy drives the current phase of accelerating cosmic expansion. Like inflation, it may decay in time to matter and radiation. However, since its energy density is minuscule in comparison, decay would be unlikely to inject such a rich variety of particles into the universe, and may instead be limited to the lowest energy fermions. Nonrelativistic neutrinos have the capacity to form stable, galaxy-engulfing haloes supported by degeneracy pressure, much like white dwarves and neutron stars. Conversely, bodies of mass 100M   can indefinitely rely on Coulomb forces for weight support. Opportunities for the mutual annihilation of electron neutrinos are largely confined to planets containing iron in the hcp phase. If dark energy decays primarily to neutrinos in 40 ~ 100 Gyr, then oceanic planets orbiting within the resulting haloes could provide long-term habitats for aquatic life with only lax constraints on the neutrino mass, 6 1 4 0m m  e V   . Various considerations now favour the possibility that neutrinos are Majorana particles with an inverted mass hierarchy and an electron neutrino mass in the vicinity of 50 meV. Sterile neutrinos of eV-mass may already be a significant component of dark matter, and could enhance planetary heating when active neutrino haloes become heavily depleted. An intriguing mechanism capable of regulating oceanic heat flux over a wide range of planetary masses is also described.

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Supersymmetric theories of neutrino dark energy

Cited by 69 publications

References 58 publications

Adiabatic instability in coupled dark energy/dark matter models

Adiabatic instability in coupled dark energy/dark matter models

Speed of sound in the mass varying neutrinos scenario

Planetary Heating by Neutrinos: Long-Term Habitats for Aquatic Life if Dark Energy Decays Favourably

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