@article{kneller_mauney_2013, title={Consequences of large theta(13) for the turbulence signatures in supernova neutrinos}, volume={88}, ISSN={["1550-2368"]}, url={http://www.scopus.com/inward/record.url?eid=2-s2.0-84881277450&partnerID=MN8TOARS}, DOI={10.1103/physrevd.88.025004}, abstractNote={Here, the transition probabilities for a single neutrino emitted from a point proto-neutron source after passage through a turbulent supernova density profile have been found to be random variates drawn from parent distributions whose properties depend upon the stage of the explosion, the neutrino energy and mixing parameters, the observed channel, and the properties of the turbulence such as the amplitude C*. In this paper we examine the consequences of the recently measured mixing angle θ13 upon the neutrino flavor transformation in supernova when passing through turbulence, in order to provide some clarity as to what one should expect in the way of turbulence effects in the next supernova neutrino burst signal. We find that the measurements of a relatively large value of θ13 means the neutrinos are relatively immune to small, C*≲1%, amplitude turbulence but as C* increases the turbulence effects grow rapidly and spread to all mixing channels. For C*≳10% the turbulence effects in the high density resonance mixing channels are independent of θ13 but nonresonant mixing channels are more sensitive to turbulence when θ13 is large.}, number={2}, journal={PHYSICAL REVIEW D}, author={Kneller, James P. and Mauney, Alex W.}, year={2013}, month={Jul} }
 @article{kneller_mauney_2013, title={Does the finite size of the proto-neutron star preclude supernova neutrino flavor scintillation due to turbulence?}, volume={88}, ISSN={["1550-2368"]}, url={http://www.scopus.com/inward/record.url?eid=2-s2.0-84884835438&partnerID=MN8TOARS}, DOI={10.1103/physrevd.88.045020}, abstractNote={Here, the transition probabilities describing the evolution of a neutrino with a given energy along some ray through a turbulent supernova profile are random variates unique to each ray. If the proto-neutron-star source of the neutrinos were a point, then one might expect the evolution of the turbulence would cause the flavor composition of the neutrinos to vary in time i.e. the flavor would scintillate. But in reality the proto-neutron star is not a point source—it has a size of order ˜10km, so the neutrinos emitted from different points at the source will each have seen different turbulence. The finite source size will reduce the correlation of the flavor transition probabilities along different trajectories and reduce the magnitude of the flavor scintillation. To determine whether the finite size of the proto-neutron star will preclude flavor scintillation, we calculate the correlation of the neutrino flavor transition probabilities through turbulent supernova profiles as a function of the separation δx between the emission points. The correlation will depend upon the power spectrum used for the turbulence, and we consider two cases: when the power spectrum is isotropic, and the more realistic case of a power spectrum which is anisotropic on large scales andmore » isotropic on small. Although it is dependent on a number of uncalibrated parameters, we show the supernova neutrino source is not of sufficient size to significantly blur flavor scintillation in all mixing channels when using an isotropic spectrum, and this same result holds when using an anisotropic spectrum, except when we greatly reduce the similarity of the turbulence along parallel trajectories separated by ˜10km or less.« less}, number={4}, journal={PHYSICAL REVIEW D}, author={Kneller, James P. and Mauney, Alex W.}, year={2013}, month={Aug} }