The 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