Abstract
Multidimensional supernova simulations indicate the presence of large scale, low multipole, asphericity generated deep within the star during the accretion phase. When density fluctuations are present in the high (H) density resonance region the neutrino flavour evolution is modified compared to the case sans turbulence. We investigate the effects of the turbulent density profiles upon the neutrinos as a function of the fluctuation amplitude and the mixing angle θ 13 and find that: turbulence effects in the H resonance channel are inevitable if θ 13 is large, and large amplitude fluctuations extend the sensitivity to θ 13 , break high-low (HL) density resonance factorization and generate non-trivial survival probabilities in the non-resonant channels.
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