We consider the supernova shock effects, the Mikheyev-Smirnov-Wolfenstein effects, the collective effects, and the Earth matter effects in the detection of type II supernova neutrinos on the Earth. It is found that the event number of supernova neutrinos depends on the neutrino mass hierarchy, the neutrino mixing angle 13 , and neutrino masses. Therefore, we propose possible methods to identify the mass hierarchy and acquire information about 13 and neutrino masses by detecting supernova neutrinos. We apply these methods to some current neutrino experiments.

The China Spallation Neutron Source (CSNS) uses H − stripping and phase space painting method to fill large ring acceptance with the linac beam of small emittance. The dependence of the painting beam on the injection beam parameters was studied for the Rapid Cycling Synchrotron (RCS) of CSNS. The injection processes for different momentum spread, rms emittance of the injection beam, injection beam matching were simulated, then the beam losses, 99% and rms emittances were obtained and the optimized ranges of injection beam parameters were given. The interaction between the H − beam and the stripping foil was studied and the foil scattering was simulated. Then, the stripping efficiency was calculated and the suitable thickness of the stripping foil was obtained. The energy deposition on the foil and the beam losses due to the foil scattering were also studied.

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.

In this paper, we first calculate the realistic Earth matter effects in the detection of type II supernova neutrinos at the Daya Bay reactor neutrino experiment which is currently under construction. It is found that the Earth matter effects depend on the neutrino incident angle θ, the neutrino mass hierarchy ∆m 2 31 , the crossing probability at the high resonance region inside the supernova, PH , the neutrino temperature, Tα, and the pinching parameter in the neutrino spectrum, ηα. We also take into account the collective effects due to neutrino-neutrino interactions inside the supernova. With the expression for the dependence of PH on the neutrino mixing angle θ13, we obtain the relations between θ13 and the event numbers for various reaction channels of supernova neutrinos. Using these relations, we propose a possible method to acquire information about θ13 smaller than 1.5• . Such a sensitivity cannot yet be achieved by the Daya Bay reactor neutrino experiment which has a sensitivity of the order of θ13 ∼ 3• . Furthermore, we apply this method to other neutrino experiments, i.e. Super-K, SNO, KamLAND, LVD, MinBooNE, Borexino, and Double-Chooz. We also study the energy spectra of the differential event numbers, dN/dE.

In this paper, we study the detection of accelerator neutrinos produced at the China Spallation Neutron Source (CSNS). Using the code FLUKA, we have simulated the production of neutrinos in the proton beam on the tungsten target and obtained the yield efficiency, numerical flux, and average energy of different flavors of neutrinos. Furthermore, detections of these accelerator neutrinos are investigated in two reaction channels, the neutrino-electron reactions and neutrino-carbon reactions. The event numbers of different flavors of neutrinos have also been calculated.