Large mixing angle solution to the solar neutrino problem and random matter density perturbations

Guzzo, M. M.; Holanda, P. C. de; Reggiani, N.

doi:10.1016/j.physletb.2003.07.010

Cited by 19 publications

(16 citation statements)

References 50 publications

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“…This topic has been widely investigated in the literature [56,57,58,59,60,61,62,63,64,65], and quantitative upper limits have already been set [61,62,63,64] by combining solar data and first KamLAND results.…”

Section: Recovering the Case Of Density Fluctuations In The Sunmentioning

confidence: 99%

Probing nonstandard decoherence effects with solar and KamLAND neutrinos

et al. 2007

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It has been speculated that quantum gravity might induce a "foamy" space-time structure at small scales, randomly perturbing the propagation phases of free-streaming particles (such as kaons, neutrons, or neutrinos). Particle interferometry might then reveal non-standard decoherence effects, in addition to standard ones (due to, e.g., finite source size and detector resolution.) In this work we discuss the phenomenology of such non-standard effects in the propagation of electron neutrinos in the Sun and in the long-baseline reactor experiment KamLAND, which jointly provide us with the best available probes of decoherence at neutrino energies E ∼ few MeV. In the solar neutrino case, by means of a perturbative approach, decoherence is shown to modify the standard (adiabatic) propagation in matter through a calculable damping factor. By assuming a power-law dependence of decoherence effects in the energy domain (E n with n = 0, ±1, ±2), theoretical predictions for two-family neutrino mixing are compared with the data and discussed. We find that neither solar nor KamLAND data show evidence in favor of non-standard decoherence effects, whose characteristic parameter γ 0 can thus be significantly constrained. In the "Lorentz-invariant" case n = −1, we obtain the upper limit γ 0 < 0.78 × 10 −26 GeV at 95% C.L. In the specific case n = −2, the constraints can also be interpreted as bounds on possible matter density fluctuations in the Sun, which we improve by a factor of ∼ 2 with respect to previous analyses.

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Section: Recovering the Case Of Density Fluctuations In The Sunmentioning

confidence: 99%

Probing nonstandard decoherence effects with solar and KamLAND neutrinos

et al. 2007

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“…One therefore clearly sees the cumulative effect characterizing neutrino propagation in random magnetic fields, implied by the sum in Eq. (23). For the simple case where all rms field amplitudes in different cells are equal to some common magnetic field value the above result gets proportional to the number of correlation cells traversed by the neutrino, N L=L 0 .…”

Section: A Simplest Random Field Modelmentioning

confidence: 88%

Enhanced solar antineutrino flux in random magnetic fields

et al. 2004

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We discuss the impact of the recent KamLAND constraint on the solar antineutrino flux on the analysis of solar neutrino data in the presence of Majorana neutrino transition magnetic moments and solar magnetic fields. We consider different stationary solar magnetic field models, both regular and random, highlighting the strong enhancement in the antineutrino production rates that characterize turbulent solar magnetic field models. Moreover, we show that for such magnetic fields inside the Sun, one can constrain the intrinsic neutrino magnetic moment down to the level of & few 10 ÿ12 B irrespective of details of the underlying turbulence model. This limit is more stringent than all current experimental sensitivities, and similar to the most stringent bounds obtained from stellar cooling. We also comment on the robustness of this limit and show that at most it might be weakened by 1 order of magnitude, under very unlikely circumstances. There is a loophole to this argument, namely, the case of Dirac neutrinos. This is certainly a particular case of the SFP Hamiltonian [4] for which the antineutrino argument does not apply. However for this case the gauge theoretic expectations for the attainable magnitudes of the transition moment are significantly lower than those for Majorana neutrinos.

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“…We will introduce the random features in the magnetic field through a delta-correlated fluctuations [18,33], which has the advantage of allowing a simple analytical parametrization of the random field in the neutrino evolution equation.…”

Section: A Magnetic Field Profilementioning

confidence: 99%

“…In other contexts of non-standard neutrino physics [18,19], we have called this region very-low LMA.…”

Section: Lma Regionmentioning

confidence: 99%

Random magnetic fields inducing solar neutrino spin-flavor precession in a three generation context

2005

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We study the effect of random magnetic fields in the spin-flavor precession of solar neutrinos in a three generation context, when a non-vanishing transition magnetic moment is assumed. While this kind of precession is strongly constrained when the magnetic moment involves the first family, such constraints do not apply if we suppose a transition magnetic moment between the second and third families. In this scenario we can have a large non-electron anti-neutrino flux arriving on Earth, which can lead to some interesting phenomenological consequences, as, for instance, the suppression of day-night asymmetry. We have analyzed the high energy solar neutrino data and the KamLAND experiment to constrain the solar mixing angle, tan θ⊙, and solar mass difference, ∆m 2 ⊙ , and we have found a larger shift of allowed values.

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Large mixing angle solution to the solar neutrino problem and random matter density perturbations

Cited by 19 publications

References 50 publications

Probing nonstandard decoherence effects with solar and KamLAND neutrinos

Probing nonstandard decoherence effects with solar and KamLAND neutrinos

Enhanced solar antineutrino flux in random magnetic fields

Random magnetic fields inducing solar neutrino spin-flavor precession in a three generation context

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