Resonant spin-flavor precession of solar and supernova neutrinos

Lim, C. S.; Marciano, William J.

doi:10.1103/physrevd.37.1368

Cited by 462 publications

(473 citation statements)

References 18 publications

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“…In general, non-diagonal elements of the magnetic moment matrix are possible and neutrinos can be changed into different flavors and chiralities [27]. Furthermore, with the additional effect of the coherent forward scattering by matter, neutrinos can be resonantly converted into those with different chiralities [28] by a mechanism similar to the well known Mikheyev-Smirnov-Wolfenstein (MSW) effect [29,30].…”

Section: Introductionmentioning

confidence: 99%

Three-generation study of neutrino spin-flavor conversion in supernovae and implication for the neutrino magnetic moment

Ando

Sato

2003

Phys. Rev. D

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We investigate resonant spin-flavor (RSF) conversions of supernova neutrinos which are induced by the interaction of neutrino magnetic moment and supernova magnetic fields. From the formulation which includes all three-flavor neutrinos and anti-neutrinos, we give a new crossing diagram that includes not only ordinary MSW resonance but also magnetically-induced RSF effect. With the diagram, it is found that four conversions occur in supernova, two are induced by the RSF effect and two by the pure MSW. We also numerically calculate neutrino conversions in supernova matter, using neutrino mixing parameters inferred from recent experimental results and a realistic supernova progenitor model. The results indicate that until 0.5 seconds after core bounce, the RSF-induced ν e ↔ ν τ transition occurs efficiently (adiabatic resonance), when µ ν > ∼ 10 −12 µ B (B 0 /5 × 10 9 G) −1 , where B 0 is the strength of the magnetic field at the surface of iron core. We also evaluate the energy spectrum as a function of µ ν B 0 at the SuperKamiokande detector and the Sudbury Neutrino Observatory using the calculated conversion probabilities, and find that the spectral deformation might have possibility to provide useful information on neutrino magnetic moment as well as magnetic field strength in supernovae.

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Section: Introductionmentioning

confidence: 99%

Three-generation study of neutrino spin-flavor conversion in supernovae and implication for the neutrino magnetic moment

Ando

Sato

2003

Phys. Rev. D

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“…The neutrino oscillation solutions to the anomaly, both matter [15] and vacuum oscillations [16], have received a great deal of attention [17]- [24] and became the most popular ones. On the other hand, the solution based on the resonance spin flavour precession (RSFP) mechanism, proposed in 1988 [25], involves the simultaneous flip of both neutrino chirality and flavour [26]. It has been much less thoroughly investigated, in particular concerning its parameter range predictions [27] and the quality of the fits involved.…”

Section: Introductionmentioning

confidence: 99%

Resonance spin flavour precession and solar neutrinos

Pulido¹,

Akhmedov²

2000

Astroparticle Physics

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We examine the prospects for the resonance spin flavour precession as a solution to the solar neutrino problem. We study seven different realistic solar magnetic field profiles and, by numerically integrating the evolution equations, perform a fit of the event rates for the three types of solar neutrino experiments (Ga, Cl and SuperKamiokande) and a fit of the energy spectrum of the recoil electrons in SuperKamiokande. A χ 2 analysis shows that the quality of the rate fits is excellent for two of the field profiles and good for all others with χ 2 /d.o.f. always well below unity. Regarding the fits for the energy spectrum, their quality is better than that for the small mixing angle MSW solution of the solar neutrino problem, at the same level as that for the large mixing angle MSW solution but worse than that for the vacuum oscillations one. The experimental data on the spectrum are however largely uncertain especially in the high energy sector, so that it is too early yet to draw any clear conclusions on the likeliest type of particle physics solution to the solar neutrino problem. *

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“…In general, nondiagonal elements of the magnetic moment matrix are possible and neutrinos can be changed into different flavours and chiralities [6]. Furthermore, with the additional effect of coherent forward scattering by matter, neutrinos can be resonantly converted into those with different chiralities [7] by a mechanism similar to the well-known MikheyevSmirnov-Wolfenstein (MSW) effect [8]. This resonant spin-flavour (RSF) conversion induced by the neutrino magnetic moment in strong magnetic fields was first introduced to solve the solar neutrino problem, and actually gave the best fit solution before the KamLAND result [9].…”

Section: Introductionmentioning

confidence: 99%

“…The RSF conversion mechanism in supernovae has been investigated by many authors [7,13,14,15]. Among them, Ando and Sato [14] have studied the RSF effect using a three-flavour formulation with the latest oscillation parameters, and pointed out that the combination of the MSW and RSF effects makes the crossing scheme very interesting to investigate.…”

Section: Introductionmentioning

confidence: 99%

A comprehensive study of neutrino spin-flavour conversion in supernovae and the neutrino mass hierarchy

Ando

Sato

2003

J. Cosmol. Astropart. Phys.

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Abstract. Resonant spin-flavour (RSF) conversions of supernova neutrinos, which is induced by the interaction between the nonzero neutrino magnetic moment and supernova magnetic fields, are studied for both normal and inverted mass hierarchy. As the case for the pure matter-induced neutrino oscillation (Mikheyev-SmirnovWolfenstein (MSW) effect), we find that the RSF transitions are strongly dependent on the neutrino mass hierarchy as well as the value of θ 13 . Flavour conversions are solved numerically for various neutrino parameter sets, with presupernova profile calculated by Woosley and Weaver. In particular, it is very interesting that the RSF-induced ν e →ν e transition occurs, if the following conditions are all satisfied: the value of µ ν B (µ ν is the neutrino magnetic moment, and B is the magnetic field strength) is sufficiently strong, the neutrino mass hierarchy is inverted, and the value of θ 13 is large enough to induce adiabatic MSW resonance. In this case, the strong peak due to original ν e emitted from neutronization burst would exist in time profile of the neutrino events detected at the Super-Kamiokande detector. If this peak were observed in reality, it would provide fruitful information on the neutrino properties. On the other hand, characters of the neutrino spectra are also different between the neutrino models, but we find that there remains degeneracy among several models. Dependence on presupernova models is also discussed.

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Resonant spin-flavor precession of solar and supernova neutrinos

Cited by 462 publications

References 18 publications

Three-generation study of neutrino spin-flavor conversion in supernovae and implication for the neutrino magnetic moment

Three-generation study of neutrino spin-flavor conversion in supernovae and implication for the neutrino magnetic moment

Resonance spin flavour precession and solar neutrinos

A comprehensive study of neutrino spin-flavour conversion in supernovae and the neutrino mass hierarchy

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