Supernova neutrino detection

By Kate Scholberg. 2000

334 citations recorded by the source corpus.

When a massive star collapses at the end of its life, nearly all of the gravitational binding energy of the resulting remnant is released in the form of neutrinos. The burst of neutrinos from a Galactic core collapse supernova will be detected in neutrino detectors worldwide. This talk will cover supernova neutrino detection techniques in general, current supernova neutrino detectors, and prospects for specific future experiments.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/bdf61d853bfcae9531e8c29231027ab548006237

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In Nuclear and High Energy Physics

Citations in the corpus

Long-Baseline Neutrino Facility (LBNF) and Deep Underground Neutrino Experiment (DUNE) Conceptual Design Report Volume 1: The LBNF and DUNE Projects (2015, background): “, water and scintillator, have the capability to record νe events [129, 130], liquid argon offers the only prospect for observation of a large, clean supernova νe sample [131].”
Current Status and Future Prospects of the SNO+ Experiment (2015, background): “[74] or a LAr target [70], provides the necessary spectral information.”
Large underground, liquid based detectors for astro-particle physics in Europe: scientific case and prospects (2007, background): “The rates of the different reaction channels are listed, and for LENA they have been obtained by scaling the predicted rates from [66, 67].”
IceCube-Gen2: the window to the extreme Universe (2020, background): “In a CCSN, 99% of the gravitational binding energy of the stellar remnant is converted into O(10 − 20) MeV neutrinos [175], and the neutrinos are thought to be important drivers of the explosion.”
Neutrino Mass Ordering from Oscillations and Beyond: 2018 Status and Future Prospects (2018, background): “(Scholberg, 2012, 2018) give an estimate of the number of neutrino events for a number of ongoing and future facilities, based on different detection techniques: water Cherenkov (including also those with long string photosensors in ice, as Icecube and PINGU), liquid argon time projection chambers,…”
Global comparison of core-collapse supernova simulations in spherical symmetry (2018, background): “5 × 10−44 cm(2), is a reference cross section for absorption of neutrinos onto nucleons [73]; Mdet is the detector mass, here taken to be the inner-volume mass of Super-Kamiokande, 32 kT [80]; mamu = 1.”
Self-induced neutrino flavor conversion without flavor mixing (2016, background): “The subsequent flavor evolution of these neutrinos influences energy deposition beyond the decoupling region, neutrino-driven nucleosynthesis, and detection opportunities of the neutrino signal from the next nearby supernova or the diffuse supernova neutrino flux from all past core-collapse events [”
Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume II: DUNE Physics (2020, background): “In the world’s current supernova neutrino flavor sensitivity portfolio [44, 42], the sensitivity is primarily to electron antineutrino flavor, via IBD.”
What can be learned from a future supernova neutrino detection (2017, background): “[80] W. P. Wright, J. P. Kneller, S. T. Ohlmann, F. K. Roepke, K. Scholberg, and I. R. Seitenzahl, “Neutrinos from Type Ia Supernovae: The Gravitationally Confined Detonation Scenario,” ArXiv e-prints, Sep. 2016.”
Long-Baseline Neutrino Facility (LBNF) and Deep Underground Neutrino Experiment (DUNE) Conceptual Design Report Volume 2: The Physics Program for DUNE at LBNF (2015, background): “, water and scintillator, have the capability to record νe events [129, 130], liquid argon offers the only prospect for observation of a large, clean supernova νe sample [131].”