Etudes des proprietes des neutrinos dans les contextes ...

tel-00450051, version 1 - 25 Jan 2010
Probability ratio
1.02
1.01
1
0.99
0.98
0 5 10 15 20
distance ( r/100 Km )
Probability ratio
1.02
1.01
1
0.99
0.98
0.5 0.6 0.7 0.8 0.9 1
distance ( r/100 Km )
Figure 6.1: Ratios of the electron neutrino oscillation probabilities for a CP
violating phase δ = 45 ◦ (dotted), 90 ◦ (dashed), 135 ◦ (dot-dashed), 180 ◦ (solid)
over δ = 0 ◦ , as a function of the distance from the neutron star surface. The
left figures shows the ratios up to 2000 km while the right figure presents the
region between 50 to 100 km where collective effects induced by the neutrino selfinteraction
are maximal. The results correspond to the case of inverted hierarchy
and small third neutrino mixing angle, for a neutrino energy of 5 MeV.
fluxes), the numerical results present significant differencies, mainly du to nonlinear
effects. In particular, their dependence with the neutrino energy still needs
to be fully understood. From the numerical results we see that the impact on
the fluxes in the star turns out to be at the level of around 10%. Several features
needs further investigation, such as the impact of the CP phase effects on Ye and
the imprint in a supernova observatory.
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