Abstract:We discuss the three neutrino flavor evolution problem with general, flavor-diagonal, matter potentials and a fully parametrized mixing matrix that includes CP violation, and derive expressions for the eigenvalues, mixing angles, and phases. We demonstrate that, in the limit that the mu and tau potentials are equal, the eigenvalues and matter mixing angles 12 and 13 are independent of the CP phase, although 23 does have CP dependence. Since we are interested in developing a framework that can be used for S mat… Show more
“…where S(E, x, t) andS(E, x, t) are the scattering matrices for neutrinos and antineutrinos respectively as discussed in [45]. Similarly H andH are the Hamiltonians for the neutrinos and antineutrinos.…”
The Matter-Neutrino Resonance (MNR) phenomenon has the potential to significantly alter the flavor content of neutrinos emitted from compact object mergers. We present the first calculations of MNR transitions using neutrino self interaction potentials and matter potentials generated selfconsistently from a dynamical model of a three-dimensional neutron star merger. In the context of the single angle approximation, we find that Symmetric and Standard MNR transitions occur in both normal and inverted hierarchy scenarios. We examine the spatial regions above the merger remnant where propagating neutrinos will encounter the matter neutrino resonance and find that a significant fraction of the neutrinos are likely to undergo MNR transitions.
“…where S(E, x, t) andS(E, x, t) are the scattering matrices for neutrinos and antineutrinos respectively as discussed in [45]. Similarly H andH are the Hamiltonians for the neutrinos and antineutrinos.…”
The Matter-Neutrino Resonance (MNR) phenomenon has the potential to significantly alter the flavor content of neutrinos emitted from compact object mergers. We present the first calculations of MNR transitions using neutrino self interaction potentials and matter potentials generated selfconsistently from a dynamical model of a three-dimensional neutron star merger. In the context of the single angle approximation, we find that Symmetric and Standard MNR transitions occur in both normal and inverted hierarchy scenarios. We examine the spatial regions above the merger remnant where propagating neutrinos will encounter the matter neutrino resonance and find that a significant fraction of the neutrinos are likely to undergo MNR transitions.
“…The CP phase δ is here set to zero. For a discussion of the conditions under which it can modify the neutrino fluxes and its possible effects see [42,46,47]. We shall explore both the normal and inverted hierarchies and consider two cases for the unknown angle θ 13 : a large value sin …”
We investigate shock wave effects upon the diffuse supernova neutrino background using dynamic profiles taken from hydrodynamical simulations and calculating the neutrino evolution in three flavors with the S-matrix formalism. We show that the shock wave impact is significant and introduces modifications of the relic fluxes by about 20% and of the associated event rates at the level of 10 − 20%. Such an effect is important since it is of the same order as the rate variation introduced when different oscillation scenarios (i.e. hierarchy or θ13) are considered. In addition, due to the shock wave, the rates become less sensitive to collective effects, in the inverted hierarchy and when sin 2 2θ13 is between the Chooz limit and 10 −5 . We propose a simplified model to account for shock wave effects in future predictions.
“…This probability can be computed from the S -matrix which relates the initial and final neutrino states by the equation |ν ′ (r ′ ) = S (r ′ , r) |ν(r) [34,35]. The S -matrix evolves according to the differential equation…”
We derive an analytical solution for the flavor evolution of a neutrino through a turbulent density profile which is found to accurately predict the amplitude and transition wavelength of numerical solutions on a case-by-case basis. The evolution is seen to strongly depend upon those Fourier modes in the turbulence which are approximately the same as the splitting between neutrino eigenvalues. Transitions are strongly enhanced by those Fourier modes in the turbulence which are approximately the same as the splitting between neutrino eigenvalues. We also find a suppression of transitions due to the long wavelength modes when the ratio of their amplitude and the wavenumber is of order, or greater than, the first root of the Bessel function J 0 .
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