The Solar Neutrino Problem

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Introduction Experiment and their results Conclusion Neutrino Oscillations A short introduction Flavor α = e, µ, τ and mass i = 1, 2, 3 eigenstates are not the same ⇒ linear combination |ν α 〉 = U αi |ν i 〉 Pontecorvo-Maki-Nakagawa-Sakata (PMNS) matrix U describes charged-current interaction (beta decay) Martin Lahrz Solar Neutrino Problem
Introduction Experiment and their results Conclusion Neutrino Oscillations A short introduction Flavor α = e, µ, τ and mass i = 1, 2, 3 eigenstates are not the same ⇒ linear combination |ν α 〉 = U αi |ν i 〉 Pontecorvo-Maki-Nakagawa-Sakata (PMNS) matrix U describes charged-current interaction (beta decay) Interference through propagation as plane wave (vacuum) |ν i (t)〉 = e −i(E i t− #» p i · #» x ) |ν i (0)〉 = e −im2 i t/2E |ν i (0)〉 leads to transition probability ( P α→β = |〈ν β (t) |ν α (0)〉| 2 ∆m ≈ sin 2 2θ sin 2 2 ) L , (α = e, β = µτ) 4E Martin Lahrz Solar Neutrino Problem
Page 1 and 2: Introduction Experiment and their r
Page 13: Introduction Experiment and their r
Page 21 and 22: Bibliography Figures Bibliography I
Page 23 and 24: Bibliography Figures Martin Lahrz S

The Solar Neutrino Problem

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