“This is something we built the detector to do,” Messier says. The energy left behind produced a particle that decayed immediately into two photons (shown in yellow and magenta) and a proton (shown in cyan). From the looks of the display, that neutrino bumped into a nucleus in the detector, transferring some of its energy but leaving no electron, muon or tau: a neutral current event. On November 12, 2013, the NOvA detector in Minnesota saw its first neutrino sent in a beam from Fermilab in Illinois. Particles can move relatively freely through this low-density material, making it easier for scientists to see what kind of message they leave behind. To combat this problem, researchers on the NOvA experiment made their detector out of light plastic. This can artificially inflate the number of electron neutrinos a physicist counts. The neutrino’s game of ring-and-run can lead to confusion, as the signal it leaves behind in a particle detector can look awfully similar to the mark of an electron neutrino, even when the particle speeding away is of another type. “Every experiment has to deal with this in one way or another,” says physicist Mark Messier of Indiana University, co-leader of the NOvA experiment. This is called a neutral current event, and, in many cases, it is the bane of the modern neutrino physicist’s existence. This lets a scientist know which flavor of neutrino dropped by.īut sometimes, the neutrino opts to play ding-dong-ditch instead, depositing a fraction of its energy in the detector before speeding away. When a neutrino shows up in a particle detector, it usually leaves a calling card in the form of an electron, a muon or a tau particle. Neutrinos come in not just one but three types, called flavors: electron, muon and tau. But detecting these tiny particles is only part of the challenge of studying them scientists also need to figure out their identities. We present the efficiency for detecting the neutrino signal depending on the supernova model and the distance to the progenitor star.Neutrinos are notoriously hard to see. Studying these neutrinos can provide information about the processes affecting the supernova explosion, probe existing supernova models, and in comparison to other neutrino experiments with different sensitivities, could answer questions about the neutrino properties as the neutrinos transit both the protoneutron star and the empty space on their way to Earth.
NOvA experiment is designed to measure neutrino oscillations in a νμ beam with average energy of 2 GeV and has little overburden, detecting interacting neutrinos with tens of MeV energy from a supernova requires dedicated data selection and background reduction. We present the efficiency for detecting the neutrino signal depending on the supernova model and the distance to the progenitor star.ĪB - This work describes a data-driven trigger designed to detect neutrino signal from a galactic supernova using the NOvA detectors. N2 - This work describes a data-driven trigger designed to detect neutrino signal from a galactic supernova using the NOvA detectors.
#NOVA NEUTRINO LICENSE#
© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-Non Commercial-No Derivatives 4.0 International License (CC BY-NC-ND 4.0). T1 - Detection of the galactic supernova neutrino signal in NOvA experiment
0 kommentar(er)
