Bulletin of the American Physical Society
2021 Fall Meeting of the APS Division of Nuclear Physics
Volume 66, Number 8
Monday–Thursday, October 11–14, 2021; Virtual; Eastern Daylight Time
Session DK: Mini-Symposium: Neutrinos and Nuclei II: Astrophysical Neutrinos and Neutrino Mass |
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Chair: Alexander Friedland, SLAC Room: Arlington |
Tuesday, October 12, 2021 9:30AM - 9:42AM |
DK.00001: Supernova Nucleosynthesis with modern Supernova Simulations Andre Sieverding, Bernhard Mueller, Yong-Zhong Qian Supernova explosions of massive stars pose a very complicated mulit-physics |
Tuesday, October 12, 2021 9:42AM - 9:54AM |
DK.00002: Production of 97Tc in Core-Collapse Supernovae Norberto Davila, Bradley S Meyer, George W Hitt, Katherine R Bermingham Core-collapse supernovae are known to produce the short-lived radionuclide 98Tc (half life of 4.2 Myr). This production is enhanced by charged-current neutrino capture reaction νe + 98Mo -> 98Tc + e- [1]. Such supernovae also produce 97Tc (half life of 4.21 Myr), and we point out that this production can be also be enhanced by the reaction νe + 98Mo -> 97Tc + e- + n. We have computed cross sections for charged-current neutrino capture on 98Tc and have estimated the branching ratio for neutron emission. We apply these cross sections to a supernova nucleosynthesis model with the result that neutrino reactions on 98Mo can increase production of 97Tc by a factor of roughly four. This enhancement may have implications for the presence of live 97Tc in the early Solar System. |
Tuesday, October 12, 2021 9:54AM - 10:06AM |
DK.00003: Prospects of supernova neutrino burst detection with COHERENT Adryanna Major All six flavors of neutrinos are ejected during core-collapse supernovae in a burst lasting tens of seconds. Since neutrinos carry away the vast majority of the explosion’s energy, detecting a core-collapse neutrino burst will give insight into the neutrino mass ordering and oscillation parameters as well as interesting astrophysics. Galactic supernova occur only a few times a century, and the neutrino community holds supernova preparedness among its chief priorities. |
Tuesday, October 12, 2021 10:06AM - 10:18AM |
DK.00004: Precision Measurements of 8B Beta Decay to Set Tensor Current Limits and Determine the Neutrino Energy Spectrum Brenden Longfellow, Aaron Gallant, Tsviki Hirsh, Mary Burkey, Jason A Clark, Guy Savard, Nicholas D Scielzo, Ralph E Segel, Louis Varriano, Daniel P Burdette, Maxime Brodeur, Daniel D Lascar, Peter Mueller, Dwaipayan Ray, Kumar S Sharma, Adrian A Valverde, Gemma L Wilson, Xinliang L Yan Studies of the beta decay of 8B provide unique sensitivity to physics beyond the Standard Model and are vital for the interpretation of solar neutrino data. A high-statistics experiment was performed at Argonne National Laboratory using the Beta-decay Paul Trap (BPT) surrounded by four double-sided silicon strip detectors to measure α and β energies from 8B → 8Be(2α) + β + ν . Through precise measurements of the kinematics of the decay products, limits on the exotic tensor current contribution to the weak interaction can be determined. At the same time, the decay product kinematics can be leveraged to reconstruct the undistorted 8B neutrino energy spectrum, a necessary ingredient for precision measurements of neutrino oscillations. Preliminary results for both the tensor current limit and the neutrino spectrum will be presented. |
Tuesday, October 12, 2021 10:18AM - 10:30AM |
DK.00005: Search for νe -16O Interactions From Low Energy Atmospheric Neutrinos in Super-Kamiokande Baran Bodur, Kate Scholberg Charged-current scattering of νe below 100 MeV from 16O nucleus is not yet measured. This interaction is a νe detection channel for water Cherenkov detectors in case of a supernova burst. Furthermore, in Super-Kamiokande diffuse supernova neutrino background (DSNB) is being searched with the inverse beta decay process and νe interactions from atmospheric neutrinos are a background to this search. Finally, atmospheric neutrinos at this energy range will be a background for the future WIMP dark matter searches via coherent elastic neutrino-nucleus scattering and νe -16O interactions are a way to probe the atmospheric νe flux at low energies to better estimate this background. A study for the first observation of this interaction from atmospheric νe with 20 years of Super-Kamiokande data is currently underway, with the goal of measuring atmospheric νe flux weighted cross section below 100 MeV. For this purpose, a custom event generator that can accurately simulate products of νe -16O and background interactions has been built. Based on the output of this event generator and detector simulations, visible energy distributions and probability of gamma and neutron emissions in Super-Kamiokande for νe -16O and background interactions are obtained. Currently statistical methods to use this information to extract number of νe -16O events in the Super-Kamiokande data are being studied. In this talk, both the event generator and the current status of the analysis will be discussed. |
Tuesday, October 12, 2021 10:30AM - 10:42AM |
DK.00006: First tritium endpoint measurement with Cyclotron Radiation Emission Spectroscopy (CRES) Talia E Weiss Project 8 aims to determine the absolute neutrino mass scale from the shape of the tritium beta decay spectrum near its endpoint. For this purpose, the collaboration developed a precise frequency-based technique for measuring electron energies: Cyclotron Radiation Emission Spectroscopy (CRES). This talk presents Project 8's analysis of the first tritium spectrum obtained with CRES. The spectrum contains 3770 events collected in 82 live days. No events were observed above the endpoint, demonstrating CRES's ultra-low background capability. We calibrate the detector response and study systematic errors using 83mKr conversion electron data. With 83mKr data taken in a shallower magnetic trap than used for tritium runs, eV-scale energy resolution was obtained—an order of magnitude from the sub-eV resolution needed for Project 8's target neutrino mass sensitivity of 40 meV. We perform Bayesian and frequentist analyses of the tritium beta spectrum, producing Project 8's first tritium endpoint measurement and neutrino mass limit. |
Tuesday, October 12, 2021 10:42AM - 10:54AM |
DK.00007: Atom-Source Development for Project 8 Alec C Lindman The Project 8 experiment will make a direct measurement with sensitivity to much of the unexplored range of neutrino masses. Past experiments used molecular tritium, which has an unavoidable energy smearing from its final states. A population of atomic tritium containing ~1020 atoms at tens of mK held in a several-cubic-meter magnetic trap will be required to reach mβ ≤ 40 meV. The efficiency of cooling the atoms and their lifetime in the trap require, coincidentally, ≥ 1020 atoms/s from the source. Phase III of Project 8 includes building an Atomic Tritium Demonstrator to confirm we are ready to produce, cool, and trap atomic tritium with methods suitable for the final Phase IV experiment. |
Tuesday, October 12, 2021 10:54AM - 11:06AM |
DK.00008: Synthetic Electron Source for Calibrating the Project 8 Neutrino Mass Experiment Andrew Ziegler Project 8 is a next-generation neutrino mass experiment that uses Cyclotron Radiation Emission Spectroscopy (CRES) to measure the neutrino mass. CRES is a novel technique for β-decay spectroscopy that measures the frequency of the cyclotron radiation produced by energetic electrons trapped in a magnetic field. The cyclotron frequency can be directly converted into the energy spectrum, which yields the neutrino mass through measurement of the spectrum endpoint. The next phase of Project 8 seeks to measure the energy spectrum of molecular tritium β-decay in an O(10 cm3) free space volume, using a multi-channel phased antenna array. I present progress on the design and fabrication of a probe antenna that mimics the electromagnetic radiation produced by an electron in a magnetic trap. The synthetic electron/CRES source will enable benchtop experiments to test the phased array reconstruction techniques necessary for performing CRES in a large volume experiment. I give an overview of the synthetic CRES antenna design and development, and show initial measurements of the gain pattern from the first prototypes. Additionally, I will outline future applications of the synthetic CRES antenna for phased array reconstruction algorithm development as well as sketch out a calibration scheme for the Project 8 phased antenna array. |
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