Etudes des proprietes des neutrinos dans les contextes ...

tel-00450051, version 1 - 25 Jan 2010
Flux (a.u.)
8e+12
6e+12
4e+12
2e+12
0
0 20 40 60 80
Neutrino Energy (MeV)
Flux (a.u.)
6e+12
4e+12
2e+12
0
0 20 40 60 80
Neutrino Energy (MeV)
Figure 4.4: Electron (left) and muon (right) neutrino fluxes Eq.(4.31) at 1000 km
from the neutron star surface, N-L (solid), N-S (dashed), I-L (dot-dashed), I-S
(dotted). In the N-L case, the first resonance is adiabatic and the Fermi-Dirac
νe distributions at the neutrino-sphere (Fig.3.3) are completely swapped with νx.
The situation is reversed for νµ. These results are obtained by fixing Tντ larger
than Tνµ by 1 MeV, as an example of the difference that could be induced by the
presence of flavor-changing interactions in the neutrino-sphere (see text).
imply that it seems hard to identify an effect of the CP-violating phase on the
number of events received in a observatory on Earth. However to draw definite
conclusions a more complete calculation needs to be performed including at least
neutrino-neutrino interactions, one loop corrections on the matter interaction,
the shock wave effects, etc...
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