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2.4 Measuring neutrino oscil<strong>la</strong>tion param<strong>et</strong>ers 23<br />

tel-00821629, version 1 - 11 May 2013<br />

three matrices M 2,3 ⇥ M 1,3 ⇥ M 1,2 :<br />

0<br />

U = @<br />

1<br />

1 0 0<br />

0 c 23 s 23<br />

A<br />

0 s 23 c 23<br />

0<br />

@<br />

c 13 0 s 13 e i 1 0<br />

0 1 0 A @<br />

c 12 s 12<br />

1<br />

0<br />

s 12 c 12 0 A<br />

0 0 1<br />

(2.16)<br />

M 2,3 is param<strong>et</strong>rized in terms of ✓ 23 which is the mixing angle dominating<br />

the ⌫ µ ! ⌫ ⌧ , re<strong>la</strong>ted to the oscil<strong>la</strong>tion of atmospheric neutrino. M 1,2 is<br />

param<strong>et</strong>rized in terms of ✓ 12 dominating the transition ⌫ e ! ⌫ µ,⌧ , re<strong>la</strong>ted<br />

to the oscil<strong>la</strong>tion of neutrino coming from the sun. Finally, M 13 <strong>de</strong>pends<br />

on ✓ 13 which is the mixing matrix dominating the oscil<strong>la</strong>tion ⌫ µ ! ⌫ e .The<br />

CP phase always appears multiplied by the terms sin ✓ 13 , so it would be<br />

measurable only if ✓ 13 is di↵erent than zero.<br />

To conclu<strong>de</strong>, the observation of the neutrino oscil<strong>la</strong>tions has two main consequences:<br />

neutrinos have a non-zero mass and the lepton f<strong>la</strong>vour is not<br />

conserved.<br />

2.4 Measuring neutrino oscil<strong>la</strong>tion param<strong>et</strong>ers<br />

To easily un<strong>de</strong>rstand neutrino oscil<strong>la</strong>tion experimental results, the simpler<br />

case with only two active neutrino is consi<strong>de</strong>red. The mixing among two<br />

neutrino families can be <strong>de</strong>scribed by a real and orthogonal 2 ⇥ 2 matrix<br />

with one mixing param<strong>et</strong>er, the rotation angle ✓ b<strong>et</strong>ween the f<strong>la</strong>vour and<br />

the mass eigenstates:<br />

✓<br />

⌫↵<br />

⌫<br />

◆ ✓ cos ✓ sin ✓<br />

=<br />

sin ✓ cos ✓<br />

The oscil<strong>la</strong>tion probability take the form:<br />

P (⌫ ↵ ! ⌫ )=sin 2 (2✓)sin 2 ✓<br />

◆✓<br />

⌫1<br />

⌫ 2<br />

◆<br />

m 2 ◆<br />

L<br />

4E<br />

(2.17)<br />

(2.18)<br />

the amplitu<strong>de</strong> of the oscil<strong>la</strong>tion, sin 2 2✓, is d<strong>et</strong>ermined by the mixing angle<br />

✓ and does not allow to distinguish b<strong>et</strong>ween ✓ and ⇡/2 ✓, which are not<br />

physically equivalent.<br />

Restoring the physics units, the oscil<strong>la</strong>tion phase becomes:<br />

✓<br />

=1.27<br />

m 2 (eV 2 ◆<br />

)L(km)<br />

E(GeV )<br />

(2.19)<br />

In the limit where ⌧ 1, P (⌫ ↵ ! ⌫ ) ' sin 2 2✓( m 2 L/(4E)) 2 ,sothe<br />

measurement of the oscil<strong>la</strong>tion probability would d<strong>et</strong>ermine information only<br />

on the pro<strong>du</strong>ct sin 2 (2✓)⇥ m 2 . The oscil<strong>la</strong>tion would not have enough time<br />

to <strong>de</strong>velop and the number of neutrino oscil<strong>la</strong>tion events measured in the

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