Sudbury neutrino observatory full#
Sudbury neutrino observatory code#

The data were taken from Phase I (1999 November-2001 May), when the detector was filled with heavy water, and Phase II (2001 July-2003 August), when NaCl was added to the target. Such bursts could indicate the detection of a nearby core-collapse supernova explosion. N2 - Results are reported from a search for low-multiplicity neutrino bursts in the Sudbury Neutrino Observatory. T1 - Low-multiplicity burst search at the Sudbury neutrino Observatory Zuber',Īharmim, B, Ahmed, SN, Anthony, AE, Barros, N, Beier, EW, Bellerive, A, Beltran, B, Bergevin, M, Biller, SD, Boudjemline, K, Boulay, MG, Cai, B, Chan, YD, Chauhan, D, Chen, M, Cleveland, BT, Dai, X, Deng, H, Detwiler, J, Doucas, G, Drouin, PL, Duncan, FA, Dunford, M, Earle, ED, Elliott, SR, Evans, HC, Ewan, GT, Farine, J, Fergani, H, Fleurot, F, Ford, RJ, Formaggio, JA, Gagnon, N, Goon, JTM, Graham, K, Guillian, E, Habib, S, Hahn, RL, Hallin, AL, Hallman, ED, Harvey, PJ, Hazama, R, Heintzelman, WJ, Heise, J, Helmer, RL, Hime, A, Howard, C, Huang, M, Jamieson, B, Jelley, NA, Jerkins, M, Klein, JR, Kos, M, Kraus, C, Krauss, CB, Kutter, T, Kyba, CCM, Law, J, Lesko, KT, Leslie, JR, Loach, JC, MacLellan, R, Majerus, S, Mak, HB, Maneira, J, Martin, R, McCauley, N, McDonald, AB, Miller, ML, Monreal, B, Monroe, J, Nickel, BG, Noble, AJ, O'keeffe, HM, Oblath, NS, Orebi Gann, GD, Oser, SM, Ott, RA, Peeters, SJM, Poon, AWP, Prior, G, Reitzner, SD, Rielage, K, Robertson, BC, Robertson, RGH, Schwendener, MH, Secrest, JA, Seibert, SR, Simard, O, Simpson, JJ, Sinclair, D, Skensved, P, Sonley, TJ, Stonehill, LC, Tešić, G, Tolich, N, Tsui, T, Van Berg, R, Van Devender, BA, Virtue, CJ, Wan Chan Tseung, H, Watson, PJS, West, N, Wilkerson, JF, Wilson, JR, Wright, A, Yeh, M, Zhang, F & Zuber, K 2011, ' Low-multiplicity burst search at the Sudbury neutrino Observatory', Astrophysical Journal, vol. It has been observed that a sequential processing of PMT hit patterns by a combination of feed-forward networks can distinguish different classes of solar neutrino events on an event-by-event basis.Īll items in the Atrium are protected by copyright with all rights reserved unless otherwise indicated.B. The usage of pattern recognition techniques with Artificial Neural Networks has been investigated for the event-type classification. Based on the results of the simulations, a simplified method to generate muon flux deep underground has been developed.

Sudbury neutrino observatory full#

Full Monte Carlo simulation of muon transport down to the SNO detector depth has been performed to understand the kinematic properties of cosmic-ray muons entering the SNO detector.

Sudbury neutrino observatory code#

In addition, the hadron transport code has been added to SNOMAN for the simulation of the secondary hadron transport and subsequent Cerenkov photon production.

In particular, the attempts to parameterize the secondary hadron multiplicity due to deep inelastic scattering are made. A model to describe muon-nucleus deep inelastic scattering is proposed. The routines describing theses processes have been implemented in the SNOMAN code to study the detector response. Muon capture and muon decay processes have been studied in detail. The processes induced by stopping muons and muon-nucleus interaction are of great importance in a water Cerenkov detector as they produce secondary particles. Secondly, the detection of high-energy atmospheric neutrinos depends on detection of muons produced by the neutrino interaction either inside the detector or in the material surrounding the detector. First, muons may produce an important source of background for solar neutrino detection. In order for the experiment to be successful, it is important to fully understand muon interactions. It is hoped that SNO will provide answers to the questions posed by the solar neutrino problem and the atmospheric neutrino anomaly. The SNO heavy water Cerenkov detector will be able to observe all three flavors of neutrinos and allow us to determine the probability of neutrino flavor oscillation. The Sudbury Neutrino Observatory (SNO) has been designed principally to study solar neutrinos and other sources of neutrinos such as supernova neutrinos and atmospheric neutrinos. Muon physics and neural network event classifier for the Sudbury Neutrino Observatory