The Solar Neutrino Problem
The Solar Neutrino Problem
The Solar Neutrino Problem
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Introduction Experiment and their results Conclusion<br />
<strong>Neutrino</strong> Oscillations<br />
Matter effects<br />
Assume two types of neutrinos. Equation of motion:<br />
i d dt |ν〉 = 1 (<br />
−<br />
∆m 2<br />
2 H |ν〉 with H = 4E cos 2θ )<br />
∆m 2<br />
4E<br />
sin 2θ<br />
∆m 2<br />
4E sin 2θ ∆m 2<br />
4E cos 2θ<br />
But: matter changes Hamiltonian<br />
(<br />
−<br />
∆m 2<br />
H = 4E cos 2θ + √ )<br />
∆m<br />
2G F N 2<br />
e 4E<br />
sin 2θ<br />
∆m 2<br />
4E sin 2θ ∆m 2<br />
4E cos 2θ<br />
⇒ resonances, Mikheev-Smirnov-Wolfenstein (MSW) effect<br />
⇒ Day/night asymmetry<br />
Martin Lahrz<br />
<strong>Solar</strong> <strong>Neutrino</strong> <strong>Problem</strong>
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