منابع مشابه
Neutrino Mass and Oscillations
The neutrino remains as exotic and challenging today as it was seventy years ago when first proposed by Pauli. What is known for certain about neutrinos is minimal indeed. They have spin 1 2 , charge 0, helicity -1, and exist in 3 flavors, electron, mu, and tau. Strictly speaking, only 2 flavors are certain: direct observation of the tau neutrino has not yet been achieved, but an experiment, DO...
متن کاملNeutrino Mass , Mixing and Oscillations
Neutrinos have been playing an important role in the evolution of our understanding of elementary particles and could have some signi cant impact on the evolution of the universe. We have strong motivations to search for non-zero neutrino mass both from theoretical and experimental aspects. Various observational data which are indicating the existence of neutrino mass and avor mixing are piling...
متن کاملSolar mass-varying neutrino oscillations.
We propose that the solar neutrino deficit may be due to oscillations of mass-varying neutrinos (MaVaNs). This scenario elucidates solar neutrino data beautifully while remaining comfortably compatible with atmospheric neutrino and K2K data and with reactor antineutrino data at short and long baselines (from CHOOZ and KamLAND). We find that the survival probability of solar MaVaNs is independen...
متن کاملAtmospheric Neutrino Oscillations, θ13 and Neutrino Mass Hierarchy
We derive predictions for the Nadir angle (θn) dependence of the ratio Nμ/Ne of the rates of the μ−like and e−like multi-GeV events measured in water-Čerenkov detectors in the case of 3-neutrino oscillations of the atmospheric νe (ν̄e) and νμ (ν̄μ), driven by one neutrino mass squared difference, |∆m31| ∼ (2.5− 3.0)× 10−3 eV2 ≫ ∆m21. This ratio is particularly sensitive to the Earth matter effect...
متن کاملElectron-Neutrino Majorana Mass and Solar Neutrino Oscillations
Assuming the Majorana masses of νe and the linear combination cντ − sνμ to be equal from their couplings to a heavy scalar triplet ξ, I show that their radiative splitting is given by ∆m2/m2ν = (3c /4π)(GF / √ 2)m2τ ln(m 2 ξ/m 2 W ). This is applicable to the small-angle matter-enhanced oscillation solution of the solar neutrino deficit and restricts mν to be between 0.20 and 0.36 eV if c 2 = 0...
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ژورنال
عنوان ژورنال: Foundations of Physics
سال: 2016
ISSN: 0015-9018,1572-9516
DOI: 10.1007/s10701-016-0040-9