Counting muons to probe the neutrino mass spectrum
Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{2...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Lujan-Peschard, Carolina [verfasserIn] Pagliaroli, Giulia [verfasserIn] Vissani, Francesco [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2013 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: The European physical journal - Berlin : Springer, 1998, 73(2013), 5 vom: 15. Mai |
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| Übergeordnetes Werk: |
volume:73 ; year:2013 ; number:5 ; day:15 ; month:05 |
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| DOI / URN: |
10.1140/epjc/s10052-013-2439-1 |
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| Katalog-ID: |
SPR008333777 |
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| 520 | |a Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. | ||
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| 700 | 1 | |a Vissani, Francesco |e verfasserin |4 aut | |
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10.1140/epjc/s10052-013-2439-1 doi (DE-627)SPR008333777 (SPR)s10052-013-2439-1-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Lujan-Peschard, Carolina verfasserin aut Counting muons to probe the neutrino mass spectrum 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. Atmospheric Neutrino (dpeaa)DE-He213 Matter Effect (dpeaa)DE-He213 Neutrino Energy (dpeaa)DE-He213 Normal Hierarchy (dpeaa)DE-He213 Inverted Hierarchy (dpeaa)DE-He213 Pagliaroli, Giulia verfasserin aut Vissani, Francesco verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 73(2013), 5 vom: 15. Mai (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:73 year:2013 number:5 day:15 month:05 https://dx.doi.org/10.1140/epjc/s10052-013-2439-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_40 GBV_ILN_63 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_206 GBV_ILN_267 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2068 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4012 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4305 GBV_ILN_4307 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4338 33.50 ASE AR 73 2013 5 15 05 |
| spelling |
10.1140/epjc/s10052-013-2439-1 doi (DE-627)SPR008333777 (SPR)s10052-013-2439-1-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Lujan-Peschard, Carolina verfasserin aut Counting muons to probe the neutrino mass spectrum 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. Atmospheric Neutrino (dpeaa)DE-He213 Matter Effect (dpeaa)DE-He213 Neutrino Energy (dpeaa)DE-He213 Normal Hierarchy (dpeaa)DE-He213 Inverted Hierarchy (dpeaa)DE-He213 Pagliaroli, Giulia verfasserin aut Vissani, Francesco verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 73(2013), 5 vom: 15. Mai (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:73 year:2013 number:5 day:15 month:05 https://dx.doi.org/10.1140/epjc/s10052-013-2439-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_40 GBV_ILN_63 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_206 GBV_ILN_267 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2068 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4012 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4305 GBV_ILN_4307 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4338 33.50 ASE AR 73 2013 5 15 05 |
| allfields_unstemmed |
10.1140/epjc/s10052-013-2439-1 doi (DE-627)SPR008333777 (SPR)s10052-013-2439-1-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Lujan-Peschard, Carolina verfasserin aut Counting muons to probe the neutrino mass spectrum 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. Atmospheric Neutrino (dpeaa)DE-He213 Matter Effect (dpeaa)DE-He213 Neutrino Energy (dpeaa)DE-He213 Normal Hierarchy (dpeaa)DE-He213 Inverted Hierarchy (dpeaa)DE-He213 Pagliaroli, Giulia verfasserin aut Vissani, Francesco verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 73(2013), 5 vom: 15. Mai (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:73 year:2013 number:5 day:15 month:05 https://dx.doi.org/10.1140/epjc/s10052-013-2439-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_40 GBV_ILN_63 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_206 GBV_ILN_267 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2068 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4012 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4305 GBV_ILN_4307 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4338 33.50 ASE AR 73 2013 5 15 05 |
| allfieldsGer |
10.1140/epjc/s10052-013-2439-1 doi (DE-627)SPR008333777 (SPR)s10052-013-2439-1-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Lujan-Peschard, Carolina verfasserin aut Counting muons to probe the neutrino mass spectrum 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. Atmospheric Neutrino (dpeaa)DE-He213 Matter Effect (dpeaa)DE-He213 Neutrino Energy (dpeaa)DE-He213 Normal Hierarchy (dpeaa)DE-He213 Inverted Hierarchy (dpeaa)DE-He213 Pagliaroli, Giulia verfasserin aut Vissani, Francesco verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 73(2013), 5 vom: 15. Mai (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:73 year:2013 number:5 day:15 month:05 https://dx.doi.org/10.1140/epjc/s10052-013-2439-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_40 GBV_ILN_63 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_206 GBV_ILN_267 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2068 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4012 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4305 GBV_ILN_4307 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4338 33.50 ASE AR 73 2013 5 15 05 |
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counting muons to probe the neutrino mass spectrum |
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Counting muons to probe the neutrino mass spectrum |
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Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. |
| abstractGer |
Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. |
| abstract_unstemmed |
Abstract The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal set-up turns out to be long baseline experiment: the muon neutrino beam, with $ 10^{20} $ protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30 %. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range. |
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Counting muons to probe the neutrino mass spectrum |
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