Detection of Supernova Neutrinos on the Earth for Large θ ₁₃

Abstract

Supernova (SN) neutrinos detected on the Earth are subject to the shock wave effects, the Mikheyev-Smirnov-Wolfenstein (MSW) effects, the neutrino collective effects and the Earth matter effects. Considering the recent experimental result about the large mixing angle θ13 (⋍ 8.8 • )provided by the Daya Bay Collaboration and applying the available knowledge for the neutrino conversion probability in the high resonance of SN, PH , which is in the form of hypergeometric function in the case of large θ13, we deduce the expression of PH taking into account the shock wave effects. It is found that PH is not zero in a certain range of time due to the shock wave effects. After considering all the four physical effects and scanning relevant parameters, we calculate the event numbers of SN neutrinos detected at the Daya Bay experiment. From the numerical results, it is found that the behaviors of neutrino event numbers detected on the Earth depend on the neutrino mass hierarchy and neutrino spectrum parameters including the temperature Tα, the dimensionless pinching parameter ηα or βα (where α refers to neutrino flavor), the average energy Eα , and the SN neutrino luminosities Lα. We also compare the results of two parametrization methods for the neutrino energy distributions and give the ranges of SN neutrino event numbers that will be detected at the Daya Bay experiment.

Current Status and Future Prospects of the SNO+ Experiment

“…The shape of the individual supernova (SN) ] (] = ] , ] , ] , where in this context ] is the sum of ] , ] , ] , and ] ) energy spectra is expected to approximate a thermal spectrum [64] in the absence of neutrino flavor changing mechanisms. At postbounce times < 1s, before shock revival, the flavor changes are expected to be reduced to those induced by the well-known MSW effect in a quasi-static environment [65,66]. At later times, many further effects interfere, significantly modifying the spectral shape.…”

Software Package for "EstrellaNueva: An Open-source Software to Study the Interactions and Detection of Neutrinos Emitted by Supernovae"

“…The rotated effective Hamiltonian H rot F allows one to construct the level diagrams shown in Figure 1, for a given neutrino energy value (Dighe & Smirnov 2000). During the first second of the burst of neutrinos from a SN, in typical SN density profiles (model independent), the neutrino evolution can be considered adiabatically (Xu et al 2014). This means that the transition probability between effective matter eigenstates can be neglected.…”

“…The software package has several SN models implemented, the adiabatic Mikheyev-Smirnov-Wolfenstein (MSW) (Dighe & Smirnov 2000;Giunti & Wook 2007;Xu et al 2014) effect for neutrino flavor transformation in the SN matter, and the analytical cross sections of the principal detection channels in current and future detectors. Another important and unique feature of this software is the option to design any target material.…”

EstrellaNueva: An Open-source Software to Study the Interactions and Detection of Neutrinos Emitted by Supernovae

“…The rotated effective Hamiltonian F rot  allows one to construct the level diagrams shown in Figure 1, for a given neutrino energy value (Dighe & Smirnov 2000). During the first second of the burst of neutrinos from a SN, in typical SN density profiles (model independent), the neutrino evolution can be considered adiabatically (Xu et al 2014). This means that the transition probability between effective matter eigenstates can be neglected.…”