Annual Review of Nuclear and Particle Science, 2009
The solar neutrino problem arose when the first measurements of the flux of neutrinos from the Su... more The solar neutrino problem arose when the first measurements of the flux of neutrinos from the Sun, taken by Raymond Davis, Jr. with a Cl-Ar radiochemical detector, fell substantially below the value predicted theoretically by John Bahcall. Bahcall's prediction came from a detailed model of the nuclear reactions powering the Sun. Resolution of the problem came three decades later with the observation of nonelectron flavors of neutrinos in the solar flux. The use of heavy water in the Sudbury Neutrino Observatory (SNO) experiment provided a means to measure both electron and nonelectron components, and the presence of the latter showed that neutrino flavor conversion was taking place—a hallmark of neutrino oscillation and mass. The solar models were vindicated, and the Standard Model of elementary particles and fields had to be revised. Here we present an account of the SNO project, its conclusions to date, and its ongoing analysis.
Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 1987
Three large sodium iodide detectors have been used to measure the pi0 electromagnetic form factor... more Three large sodium iodide detectors have been used to measure the pi0 electromagnetic form factor. The manner in which they were operated is described here with particular emphasis on optimizing energy resolution, measuring response functions and acceptance, and precise energy calibration. Neutron rejection by pulse shape discrimination was also investigated.
The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an inte... more The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this document, the product of a workshop at the SNS in May 2012, we describe this free, high-quality stopped-pion neutrino source and outline various physics that could be done using it. We describe without prioritization some specific experimental configurations that could address these physics topics.
At the end of a massive star’s life, a violent explosion known as a supernova occurs and releases... more At the end of a massive star’s life, a violent explosion known as a supernova occurs and releases 99% of the star’s gravitational binding energy in the form of neutrinos. Although the explosion generates a huge burst of neutrinos, the large distance to earthbound detectors, low cross sections, and flavour changing oscillations can make detection and analysis challenging. Only one neutrino burst from a supernova has ever been detected, but neutrino detectors have been waiting patiently for another. The SNO+ detector at SNOLAB can be used as a supernova detector during both regular operation and calibrations by measuring the burst of neutrinos from a supernova. We present the neutrino detection method and analysis of potential galactic supernova with the SNO+ detector.
AbstractThe Helium and Lead Observatory (HALO) is a dedicated supernova detector constructed in ... more AbstractThe Helium and Lead Observatory (HALO) is a dedicated supernova detector constructed in the underground facilities at SNOLAB in Sudbury, Canada. It is designed to detect neutrinos from a supernova within the Milky Way galaxy using lead blocks and 3He neutron ...
The probability of pion capture by hydrogen was measured for CH3OH, CD3OH, and CH3OD as a functio... more The probability of pion capture by hydrogen was measured for CH3OH, CD3OH, and CH3OD as a function of temperature from -150 to +250 °C. The nuclear capture of a pion by a proton was identified using the pion charge-exchange reaction. The coincident photons from the pi0 decay were detected by TRIUMF's large NaI spectrometers. We have found a relative difference
Annual Review of Nuclear and Particle Science, 2009
The solar neutrino problem arose when the first measurements of the flux of neutrinos from the Su... more The solar neutrino problem arose when the first measurements of the flux of neutrinos from the Sun, taken by Raymond Davis, Jr. with a Cl-Ar radiochemical detector, fell substantially below the value predicted theoretically by John Bahcall. Bahcall's prediction came from a detailed model of the nuclear reactions powering the Sun. Resolution of the problem came three decades later with the observation of nonelectron flavors of neutrinos in the solar flux. The use of heavy water in the Sudbury Neutrino Observatory (SNO) experiment provided a means to measure both electron and nonelectron components, and the presence of the latter showed that neutrino flavor conversion was taking place—a hallmark of neutrino oscillation and mass. The solar models were vindicated, and the Standard Model of elementary particles and fields had to be revised. Here we present an account of the SNO project, its conclusions to date, and its ongoing analysis.
Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 1987
Three large sodium iodide detectors have been used to measure the pi0 electromagnetic form factor... more Three large sodium iodide detectors have been used to measure the pi0 electromagnetic form factor. The manner in which they were operated is described here with particular emphasis on optimizing energy resolution, measuring response functions and acceptance, and precise energy calibration. Neutron rejection by pulse shape discrimination was also investigated.
The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an inte... more The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this document, the product of a workshop at the SNS in May 2012, we describe this free, high-quality stopped-pion neutrino source and outline various physics that could be done using it. We describe without prioritization some specific experimental configurations that could address these physics topics.
At the end of a massive star’s life, a violent explosion known as a supernova occurs and releases... more At the end of a massive star’s life, a violent explosion known as a supernova occurs and releases 99% of the star’s gravitational binding energy in the form of neutrinos. Although the explosion generates a huge burst of neutrinos, the large distance to earthbound detectors, low cross sections, and flavour changing oscillations can make detection and analysis challenging. Only one neutrino burst from a supernova has ever been detected, but neutrino detectors have been waiting patiently for another. The SNO+ detector at SNOLAB can be used as a supernova detector during both regular operation and calibrations by measuring the burst of neutrinos from a supernova. We present the neutrino detection method and analysis of potential galactic supernova with the SNO+ detector.
AbstractThe Helium and Lead Observatory (HALO) is a dedicated supernova detector constructed in ... more AbstractThe Helium and Lead Observatory (HALO) is a dedicated supernova detector constructed in the underground facilities at SNOLAB in Sudbury, Canada. It is designed to detect neutrinos from a supernova within the Milky Way galaxy using lead blocks and 3He neutron ...
The probability of pion capture by hydrogen was measured for CH3OH, CD3OH, and CH3OD as a functio... more The probability of pion capture by hydrogen was measured for CH3OH, CD3OH, and CH3OD as a function of temperature from -150 to +250 °C. The nuclear capture of a pion by a proton was identified using the pion charge-exchange reaction. The coincident photons from the pi0 decay were detected by TRIUMF's large NaI spectrometers. We have found a relative difference
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