Earth matter effects in supernova neutrinos: Optimal detector locations
A model-independent experimental signature for flavor oscillations in the neutrino signal from the next Galactic supernova (SN) would be the observation of Earth matter effects. We calculate the probability for observing a Galactic SN shadowed by the Earth as a function of the detector's geogra...
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ftdatacite:10.48550/arxiv.astro-ph/0604300 2023-05-15T18:22:13+02:00 Earth matter effects in supernova neutrinos: Optimal detector locations Mirizzi, A. Raffelt, G. G. Serpico, P. D. 2006 https://dx.doi.org/10.48550/arxiv.astro-ph/0604300 https://arxiv.org/abs/astro-ph/0604300 unknown arXiv https://dx.doi.org/10.1088/1475-7516/2006/05/012 Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ Astrophysics astro-ph High Energy Physics - Experiment hep-ex High Energy Physics - Phenomenology hep-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 2006 ftdatacite https://doi.org/10.48550/arxiv.astro-ph/0604300 https://doi.org/10.1088/1475-7516/2006/05/012 2022-04-01T15:44:22Z A model-independent experimental signature for flavor oscillations in the neutrino signal from the next Galactic supernova (SN) would be the observation of Earth matter effects. We calculate the probability for observing a Galactic SN shadowed by the Earth as a function of the detector's geographic latitude. This probability depends only mildly on details of the Galactic SN distribution. A location at the North Pole would be optimal with a shadowing probability of about 60%, but a far-northern location such as Pyhasalmi in Finland, the proposed site for a large-volume scintillator detector, is almost equivalent (58%). We also consider several pairs of detector locations and calculate the probability that only one of them is shadowed, allowing a comparison between a shadowed and a direct signal. For the South Pole combined with Kamioka this probability is almost 75%, for the South Pole combined with Pyhasalmi it is almost 90%. One particular scenario consists of a large-volume scintillator detector located in Pyhasalmi to measure the geo-neutrino flux in a continental location and another such detector in Hawaii to measure it in an oceanic location. The probability that only one of them is shadowed exceeds 50% whereas the probability that at least one is shadowed is about 80%. We provide an online tool to calculate different shadowing probabilities for the one- and two-detector cases. : v2: 17 pages, 6 eps figures. Typos removed, matches the published version. Online tool to calculate the Earth shadowing probabilities available at http://www.mppmu.mpg.de/supernova/shadowing . High-resolution color version of fig_2a and fig_2b available at http://www.mppmu.mpg.de/supernova/shadowing/map Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole North Pole |
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Astrophysics astro-ph High Energy Physics - Experiment hep-ex High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
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Astrophysics astro-ph High Energy Physics - Experiment hep-ex High Energy Physics - Phenomenology hep-ph FOS Physical sciences Mirizzi, A. Raffelt, G. G. Serpico, P. D. Earth matter effects in supernova neutrinos: Optimal detector locations |
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Astrophysics astro-ph High Energy Physics - Experiment hep-ex High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
description |
A model-independent experimental signature for flavor oscillations in the neutrino signal from the next Galactic supernova (SN) would be the observation of Earth matter effects. We calculate the probability for observing a Galactic SN shadowed by the Earth as a function of the detector's geographic latitude. This probability depends only mildly on details of the Galactic SN distribution. A location at the North Pole would be optimal with a shadowing probability of about 60%, but a far-northern location such as Pyhasalmi in Finland, the proposed site for a large-volume scintillator detector, is almost equivalent (58%). We also consider several pairs of detector locations and calculate the probability that only one of them is shadowed, allowing a comparison between a shadowed and a direct signal. For the South Pole combined with Kamioka this probability is almost 75%, for the South Pole combined with Pyhasalmi it is almost 90%. One particular scenario consists of a large-volume scintillator detector located in Pyhasalmi to measure the geo-neutrino flux in a continental location and another such detector in Hawaii to measure it in an oceanic location. The probability that only one of them is shadowed exceeds 50% whereas the probability that at least one is shadowed is about 80%. We provide an online tool to calculate different shadowing probabilities for the one- and two-detector cases. : v2: 17 pages, 6 eps figures. Typos removed, matches the published version. Online tool to calculate the Earth shadowing probabilities available at http://www.mppmu.mpg.de/supernova/shadowing . High-resolution color version of fig_2a and fig_2b available at http://www.mppmu.mpg.de/supernova/shadowing/map |
format |
Text |
author |
Mirizzi, A. Raffelt, G. G. Serpico, P. D. |
author_facet |
Mirizzi, A. Raffelt, G. G. Serpico, P. D. |
author_sort |
Mirizzi, A. |
title |
Earth matter effects in supernova neutrinos: Optimal detector locations |
title_short |
Earth matter effects in supernova neutrinos: Optimal detector locations |
title_full |
Earth matter effects in supernova neutrinos: Optimal detector locations |
title_fullStr |
Earth matter effects in supernova neutrinos: Optimal detector locations |
title_full_unstemmed |
Earth matter effects in supernova neutrinos: Optimal detector locations |
title_sort |
earth matter effects in supernova neutrinos: optimal detector locations |
publisher |
arXiv |
publishDate |
2006 |
url |
https://dx.doi.org/10.48550/arxiv.astro-ph/0604300 https://arxiv.org/abs/astro-ph/0604300 |
geographic |
South Pole North Pole |
geographic_facet |
South Pole North Pole |
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South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.1088/1475-7516/2006/05/012 |
op_rights |
Assumed arXiv.org perpetual, non-exclusive license to distribute this article for submissions made before January 2004 http://arxiv.org/licenses/assumed-1991-2003/ |
op_doi |
https://doi.org/10.48550/arxiv.astro-ph/0604300 https://doi.org/10.1088/1475-7516/2006/05/012 |
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1766201594665238528 |