High-energy neutrinos flavor composition as a probe of neutrino magnetic moments

Neutrino propagation in the Galactic and extragalactic magnetic fields is considered. We extend an approach developed in [A. Popov and A. Studenikin, Neutrino eigenstates and flavour, spin and spin-flavour oscillations in a constant magnetic field, .] to describe neutrino flavor and spin oscillations using wave packets. The evolution equations for the neutrino wave packets in a uniform and nonuniform magnetic fields are derived. The analytical expressions for neutrino flavor and spin oscillations probabilities accounting for damping due to the wave packet separation are obtained for the case of a uniform magnetic field. It is shown that terms in the flavor oscillations probabilities that depend on the magnetic field strength are characterized by two coherence lengths. One of the coherence lengths coincides with the coherence length for neutrino oscillations in vacuum, while the second one is proportional to the cube of the average neutrino momentum <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:msubsup><a:mi>p</a:mi><a:mn>0</a:mn><a:mn>3</a:mn></a:msubsup></a:math>. The probabilities of flavor and spin oscillations are calculated numerically for neutrino interacting with the nonuniform Galactic magnetic field. It is shown that oscillations on certain frequencies are suppressed on the Galactic scale due to the neutrino wave packets separation. The flavor compositions of high-energy neutrino flux coming from the Galactic center and ultra-high energy neutrinos from an extragalactic source are calculated accounting for neutrino interaction with the magnetic field and decoherence due to the wave packet separation. It is shown that for neutrino magnetic moments <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mo>∼</c:mo><c:msup><c:mn>10</c:mn><c:mrow><c:mo>−</c:mo><c:mn>13</c:mn></c:mrow></c:msup><c:msub><c:mi>μ</c:mi><c:mi>B</c:mi></c:msub></c:math> and larger these flavor compositions significantly differ from ones predicted by the vacuum neutrino oscillations scenario.