Resonant amplification of ν oscillations in matter and solar-neutrino spectroscopy

Mikheyev, S.; Smirnov, A. Yu.

doi:10.1007/bf02508049

Cited by 1,391 publications

(708 citation statements)

References 7 publications

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“…(1) we omitted a term proportional to the identity (this includes the other Wolfenstein potential V n (x) = −(1/ √ 2)G F N n (x) describing the neutral-current interaction of neutrinos with neutrons). The presence of the Mikheev, Smirnov, Wolfenstein (MSW) resonance [23,24,25] is manifest in the first term.…”

Section: Second-quantized Formalismmentioning

confidence: 99%

Neutrino–neutrino interactions and flavour mixing in dense matter

Balantekin

Pehlivan

2006

J. Phys. G: Nucl. Part. Phys.

128

130

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An algebraic approach to the neutrino propagation in dense media is presented. The Hamiltonian describing a gas of neutrinos interacting with each other and with background fermions is written in terms of the appropriate SU(N) operators, where N is the number of neutrino flavors. The evolution of the resulting many-body problem is formulated as a coherent-state path integral. Some commonly used approximations are shown to represent the saddle-point solution of the path integral for the full many-body system.

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Section: Second-quantized Formalismmentioning

confidence: 99%

Neutrino–neutrino interactions and flavour mixing in dense matter

Balantekin

Pehlivan

2006

J. Phys. G: Nucl. Part. Phys.

128

130

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“…The concequences of this difference will be seen in the allowed regions behaviour in the neutrino oscillation parameter space. In our analysis, we find results numerically by diagonalizing the Hamiltonian in equation (2). The relevant method was discussed in [5].…”

Section: Evolution Equation For Majorana Neutrinos In the Rsfp Frameworkmentioning

confidence: 99%

“…where ν e → ν µ transition probability P (ν e → ν µ ; SF P ) is calculated numerically from the equation (2). P (ν µ → ν e ; V acuumOsc.)…”

Section: Solar Electron Antineutrino Fluxmentioning

confidence: 99%

Global analysis of solar neutrinos (assumed to be Majorana particles) together with the new KamLAND data in the RSFP framework

Yılmaz

Yılmazer

2005

J. Phys. G: Nucl. Part. Phys.

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Assuming neutrinos are Majorana particles having non-zero transitionmagnetic moments, a global analysis of solar neutrino data, together with the new KamLAND data, is presented in the resonant spin flavor precession (RSFP) framework. We used Wood-Saxon and Gaussian shaped magnetic field profiles throughout the entire Sun. For each magnetic field profile, allowed regions from solar data combined with new KamLAND data are examined at 95% confidence level (CL). We showed that all allowed regions are in the large mixing angle (LMA) region and remain the same as the µB value is increased for both magnetic field profiles, contrary to the Dirac case studied in our previous work. The electron antineutrino flux from the Sun is calculated, and via the results obtained several limits are set for µB. 1.IntroductionThe magnetic moment solution to solar neutrino problem is alternative possible mechanism to MSW [1 − 2] neutrino oscillation solutions. In this solution motivated by Okun et al (OVV) [3], strong magnetic field in the Sun changes neutrino's helicity which has non-zero transition magnetic moment, as it passes through a region with the magnetic field. Shortly after this solution was proposed, resonance spin flavor precession (RSFP) was proposed by Lim and Marciano [4]. In the RSFP scenario, there is a combined effect of matter and magnetic field in the Sun on neutrino's spin and flavor precession. Thus, the neutrino's spin and flavor flip simultaneously. In other words, left-handed electron neutrinos convert to right-handed neutrinos of other types: In this work, assuming the fact that all neutrinos are Majorana particles, we present a global analysis of solar data combined with the new KamLAND data [12] in the RSFP scenario. We obtain allowed regions by using standart least squares analysis on the oscillation parameter space, ∆m 2 and tan 2 θ, space. Our results showed that all allowed regions are in the large mixing angle (LMA) region and have the same chi-square value as µB value is increased for both magnetic field profiles. After the combined analysis of solar and KamLAND data, we examine the electron antineutrino flux at certain ∆m 2 and tan 2 θ values.This paper is divided as fallows: in section 2 we give general information on the evolution equation of Majorana neutrinos having transition magnetic moment. In section 3 the relevant magnetic field profiles are given. Detailed statistical analysis are given in section 4. In section 5 a theoretical framework is given for the calculation of the solar antineutrino flux. Finally, our results and conclusion are presented in section 6. Evolution equation for Majorana neutrinos in the RSFP frameworkFor two generations, Majorana neutrino flavors are ν e , ν µ , ν e , ν µ . Altough Dirac neutrinos have diagonal and off-diagonal magnetic moments, Majorana neutrinos have only off-diagonal (transition) magnetic moments. For the Majorana neutrinos that propagate through matter and in a transverse magnetic field B, the evolution equation in the case of two generations...

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“…Strictly speaking one should consider the helicity states ν ± (that are mass eigenstates) in (47), however at high energies ν L ≃ ν − , ν R ≃ ν + . Assuming that m 1 = m 2 , taking p 1 ∼ p 2 along the x 3 -axis and substituting (47) into the Schroedinger equation that corresponds to H e , one obtains…”

Section: Neutrino Helicity Oscillationsmentioning

confidence: 99%

Quantum Systems in Weak Gravitational Fields

Papini

2002

Advances in the Interplay Between Quantum and Gravity Physics

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Resonant amplification of ν oscillations in matter and solar-neutrino spectroscopy

Cited by 1,391 publications

References 7 publications

Neutrino–neutrino interactions and flavour mixing in dense matter

Neutrino–neutrino interactions and flavour mixing in dense matter

Global analysis of solar neutrinos (assumed to be Majorana particles) together with the new KamLAND data in the RSFP framework

Quantum Systems in Weak Gravitational Fields

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