We investigate toy models for spatial and temporal instabilities in collective neutrino oscillations induced by self-interactions, with special emphasis on inhomogeneous systems densities following a profile. Simulations are based mathematica program that solves the Liouville equation or without vacuum terms, refractive terms from background medium, neutrino-neutrino forward scattering, one spa...

We quantify the amount of data needed in order to measure the size and position of the ^{8}B neutrino production region within the solar core, for experiments looking at elastic scattering between electrons and solar neutrinos. The directions of the electrons immediately after scattering are strongly correlated with the incident directions of the neutrinos; however, this is degraded significant...

John N. Bahcall∗ School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540 Plamen I. Krastev† Department of Physics, University of Wisconsin, Madison, WI 53706 Alexei Yu. Smirnov‡ International Center for Theoretical Physics, 34100 Trieste, Italy We calculate the range of predicted values for 10 quantities that will be measured by the Sudbury Neutrino Observatory (SNO). We u...

Neutrino-neutrino refraction dominates the flavor evolution in core-collapse supernovae, neutron-star mergers, and early universe. Ordinary neutrino conversion develops on timescales determined by vacuum oscillation frequency. However, when density is large enough, collective may arise because of pairwise scattering. Pairwise deemed to be fast as it expected occur that depend neutrino-neutrino ...

We calculate neutrino cross sections from neutral current reactions in the dense matter encountered in the evolution of a newly born neutron star. Effects of composition and of strong interactions in the deleptonization and cooling phases of the evolution are studied. The influence of the possible presence of strangeness-rich hyperons on the neutrino scattering cross sections is explored. Due t...

The ANTARES deep-sea neutrino telescope comprises a three-dimensional array of photomultipliers to detect the Cherenkov light induced by upgoing relativistic charged particles originating from neutrino interactions in the vicinity of the detector. The large scattering length of light in the deep sea facilitates an angular resolution of a few tenths of a degree for neutrino energies exceeding 10...