MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations
Abstract. 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 g...
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ftciteseerx:oai:CiteSeerX.psu:10.1.1.257.3134 2023-05-15T17:39:56+02:00 MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations A. Mirizzi G. G. Raffelt P. D. Serpico The Pennsylvania State University CiteSeerX Archives 2006 application/pdf http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.3134 http://arxiv.org/pdf/astro-ph/0604300v2.pdf en eng http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.3134 http://arxiv.org/pdf/astro-ph/0604300v2.pdf Metadata may be used without restrictions as long as the oai identifier remains attached to it. http://arxiv.org/pdf/astro-ph/0604300v2.pdf Supernova neutrinos neutrino detectors text 2006 ftciteseerx 2016-01-07T19:59:59Z Abstract. 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 Pyhäsalmi in Finland, the proposed site for a largevolume 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 Pyhäsalmi it is almost 90%. One particular scenario consists of a largevolume scintillator detector located in Pyhäsalmi 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. Text North Pole South pole Unknown North Pole South Pole |
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Supernova neutrinos neutrino detectors |
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Supernova neutrinos neutrino detectors A. Mirizzi G. G. Raffelt P. D. Serpico MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations |
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Supernova neutrinos neutrino detectors |
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Abstract. 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 Pyhäsalmi in Finland, the proposed site for a largevolume 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 Pyhäsalmi it is almost 90%. One particular scenario consists of a largevolume scintillator detector located in Pyhäsalmi 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. |
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The Pennsylvania State University CiteSeerX Archives |
format |
Text |
author |
A. Mirizzi G. G. Raffelt P. D. Serpico |
author_facet |
A. Mirizzi G. G. Raffelt P. D. Serpico |
author_sort |
A. Mirizzi |
title |
MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations |
title_short |
MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations |
title_full |
MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations |
title_fullStr |
MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations |
title_full_unstemmed |
MPP-2006-28 Earth matter effects in supernova neutrinos: Optimal detector locations |
title_sort |
mpp-2006-28 earth matter effects in supernova neutrinos: optimal detector locations |
publishDate |
2006 |
url |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.3134 http://arxiv.org/pdf/astro-ph/0604300v2.pdf |
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North Pole South Pole |
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North Pole South Pole |
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North Pole South pole |
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North Pole South pole |
op_source |
http://arxiv.org/pdf/astro-ph/0604300v2.pdf |
op_relation |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.257.3134 http://arxiv.org/pdf/astro-ph/0604300v2.pdf |
op_rights |
Metadata may be used without restrictions as long as the oai identifier remains attached to it. |
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1766140700410249216 |