OperaV1, PascalFrancis, Corpus, bibRecord, 000076

BEAMING NEUTRINOS AND ANTI-NEUTRINOS ACROSS THE EARTH TO DISENTANGLE NEUTRINO MIXING PARAMETERS

Identifieur interne : 000076 ( PascalFrancis/Corpus ); précédent : 000075; suivant : 000077

BEAMING NEUTRINOS AND ANTI-NEUTRINOS ACROSS THE EARTH TO DISENTANGLE NEUTRINO MIXING PARAMETERS

Auteurs : Daniele Fargion ; Daniele D'Armiento ; Paolo Desiati ; Paolo Paggi

Source :

The Astrophysical journal [ 0004-637X ] ; 2012.

RBID : Pascal:12-0410344

Descripteurs français

Pascal (Inist)
- Neutrino muonique, Mélangeage, Violation parité, Invariance CPT, Lepton tau, Flaveur, Hiérarchie, Masse neutrino, Anisotropie, Asymétrie, Oscillation neutrino, Diamètre, CERN, Courant neutre, Matrice détecteur, Rayonnement cosmique, Nucléosynthèse, Abondance, Particule sans masse, Masse particule élémentaire, Particule élémentaire.

English descriptors

KwdEn :
- Abundance, Anisotropy, Asymmetry, CERN, CPT invariance, Cosmic radiation, Dectector arrays, Diameter, Elementary particle mass, Elementary particles, Flavor, Hierarchy, Massless particles, Mixing, Muon neutrinos, Neutral currents, Neutrino mass, Neutrino oscillations, Nucleosynthesis, Parity violation, Tau leptons.

Abstract

A result from MINOS seemed to indicate that the mass splitting and mixing angle of anti-neutrinos is different from that of neutrinos, suggesting a charge-parity-time (CPT) violation in the lepton sector. However, more recent MINOS data reduced the ν_μ-ν_μ differences leading to a narrow discrepancy nearly compatible with no CPT violation. However, the last few years of OPERA activity on the appearance of a tau lepton (one unique event) still has not been probed and more tools may be required to disentangle a list of parameters (μ-τ flavor mixing, tau appearance, any eventual CPT violation, θ₁₃ angle value, and any hierarchy neutrino mass). Atmospheric anisotropy in muon neutrino spectra in the DeepCore, at ten to tens of GeV (unpublished), can hardly reveal asymmetry in the eventual ν_μ-ν_μ oscillation parameters. Here we considered how the longest baseline neutrino oscillation available, crossing most of Earth's diameter, may improve the measurement and at best disentangle any hypothetical CPT violation occurring between the earliest (2010) and the present (2012) MINOS bounds (with 6σ a year), while testing τ and even the appearance of τ at the highest rate. The ν_μ and ν_μ disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of ν_μ and ν_μ crossing through the Earth, within an OPERA-like experiment from CERN (or Fermilab), in the direction of the IceCube-DeepCore ν detector at the South Pole. The ideal energy lies at 21 GeV to test the disappearance or (for any tiny CPT violation) the partial ν_μ appearance. Such a tuned detection experiment may lead to a strong signature of τ or τ generation even within its neutral current noise background events: nearly one τ or two τ a day. The tau appearance signal is above (or within) 10σ a year, even for a 1% OPERA-like experiment. Peculiar configurations for θ₁₃ and the hierarchy neutrino mass test may also be better addressed by a DeepCore-PINGU array detector beaming ν_μ and observing ν_e at 6 GeV neutrino energy windows.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A02	`01`			`@0 ASJOAB`
A03		`1`		`@0 Astrophys. j.`
A05				`@2 758`
A06				`@2 1 @3 p. 1`
A08	`01`	`1`	`ENG`	`@1 BEAMING NEUTRINOS AND ANTI-NEUTRINOS ACROSS THE EARTH TO DISENTANGLE NEUTRINO MIXING PARAMETERS`
A11	`01`	`1`		`@1 FARGION (Daniele)`
A11	`02`	`1`		`@1 D'ARMIENTO (Daniele)`
A11	`03`	`1`		`@1 DESIATI (Paolo)`
A11	`04`	`1`		`@1 PAGGI (Paolo)`
A14	`01`			`@1 Physics Department, Rome University 1, P.le A Moro 5 @2 00185 Rome @3 ITA @Z 1 aut. @Z 2 aut. @Z 4 aut.`
A14	`02`			`@1 INFN Sezione di Roma, Roma 1 @2 00185, Roma @3 ITA @Z 1 aut.`
A14	`03`			`@1 Department of Physics, University of Wisconsin-Madison, 1150 University Avenue Madison @2 WI 53706 @3 USA @Z 3 aut.`
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A61				`@0 A`
A64	`01`	`1`		`@0 The Astrophysical journal`
A66	`01`			`@0 GBR`
C01	`01`		`ENG`	@0 A result from MINOS seemed to indicate that the mass splitting and mixing angle of anti-neutrinos is different from that of neutrinos, suggesting a charge-parity-time (CPT) violation in the lepton sector. However, more recent MINOS data reduced the ν_μ-ν_μ differences leading to a narrow discrepancy nearly compatible with no CPT violation. However, the last few years of OPERA activity on the appearance of a tau lepton (one unique event) still has not been probed and more tools may be required to disentangle a list of parameters (μ-τ flavor mixing, tau appearance, any eventual CPT violation, θ₁₃ angle value, and any hierarchy neutrino mass). Atmospheric anisotropy in muon neutrino spectra in the DeepCore, at ten to tens of GeV (unpublished), can hardly reveal asymmetry in the eventual ν_μ-ν_μ oscillation parameters. Here we considered how the longest baseline neutrino oscillation available, crossing most of Earth's diameter, may improve the measurement and at best disentangle any hypothetical CPT violation occurring between the earliest (2010) and the present (2012) MINOS bounds (with 6σ a year), while testing τ and even the appearance of τ at the highest rate. The ν_μ and ν_μ disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of ν_μ and ν_μ crossing through the Earth, within an OPERA-like experiment from CERN (or Fermilab), in the direction of the IceCube-DeepCore ν detector at the South Pole. The ideal energy lies at 21 GeV to test the disappearance or (for any tiny CPT violation) the partial ν_μ appearance. Such a tuned detection experiment may lead to a strong signature of τ or τ generation even within its neutral current noise background events: nearly one τ or two τ a day. The tau appearance signal is above (or within) 10σ a year, even for a 1% OPERA-like experiment. Peculiar configurations for θ₁₃ and the hierarchy neutrino mass test may also be better addressed by a DeepCore-PINGU array detector beaming ν_μ and observing ν_e at 6 GeV neutrino energy windows.
C02	`01`	`3`		`@0 001E03`
C03	`01`	`3`	`FRE`	`@0 Neutrino muonique @5 26`
C03	`01`	`3`	`ENG`	`@0 Muon neutrinos @5 26`
C03	`02`	`3`	`FRE`	`@0 Mélangeage @5 27`
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C03	`03`	`X`	`FRE`	`@0 Violation parité @5 28`
C03	`03`	`X`	`ENG`	`@0 Parity violation @5 28`
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C03	`04`	`3`	`ENG`	`@0 CPT invariance @5 29`
C03	`05`	`3`	`FRE`	`@0 Lepton tau @5 30`
C03	`05`	`3`	`ENG`	`@0 Tau leptons @5 30`
C03	`06`	`3`	`FRE`	`@0 Flaveur @5 31`
C03	`06`	`3`	`ENG`	`@0 Flavor @5 31`
C03	`07`	`X`	`FRE`	`@0 Hiérarchie @5 32`
C03	`07`	`X`	`ENG`	`@0 Hierarchy @5 32`
C03	`07`	`X`	`SPA`	`@0 Jerarquía @5 32`
C03	`08`	`3`	`FRE`	`@0 Masse neutrino @5 33`
C03	`08`	`3`	`ENG`	`@0 Neutrino mass @5 33`
C03	`09`	`3`	`FRE`	`@0 Anisotropie @5 34`
C03	`09`	`3`	`ENG`	`@0 Anisotropy @5 34`
C03	`10`	`3`	`FRE`	`@0 Asymétrie @5 35`
C03	`10`	`3`	`ENG`	`@0 Asymmetry @5 35`
C03	`11`	`3`	`FRE`	`@0 Oscillation neutrino @5 36`
C03	`11`	`3`	`ENG`	`@0 Neutrino oscillations @5 36`
C03	`12`	`X`	`FRE`	`@0 Diamètre @5 37`
C03	`12`	`X`	`ENG`	`@0 Diameter @5 37`
C03	`12`	`X`	`SPA`	`@0 Diámetro @5 37`
C03	`13`	`3`	`FRE`	`@0 CERN @5 38`
C03	`13`	`3`	`ENG`	`@0 CERN @5 38`
C03	`14`	`3`	`FRE`	`@0 Courant neutre @5 39`
C03	`14`	`3`	`ENG`	`@0 Neutral currents @5 39`
C03	`15`	`3`	`FRE`	`@0 Matrice détecteur @5 40`
C03	`15`	`3`	`ENG`	`@0 Dectector arrays @5 40`
C03	`16`	`3`	`FRE`	`@0 Rayonnement cosmique @5 41`
C03	`16`	`3`	`ENG`	`@0 Cosmic radiation @5 41`
C03	`17`	`3`	`FRE`	`@0 Nucléosynthèse @5 42`
C03	`17`	`3`	`ENG`	`@0 Nucleosynthesis @5 42`
C03	`18`	`3`	`FRE`	`@0 Abondance @5 43`
C03	`18`	`3`	`ENG`	`@0 Abundance @5 43`
C03	`19`	`3`	`FRE`	`@0 Particule sans masse @5 44`
C03	`19`	`3`	`ENG`	`@0 Massless particles @5 44`
C03	`20`	`3`	`FRE`	`@0 Masse particule élémentaire @5 45`
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N21				`@1 317`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 12-0410344 INIST
ET :	BEAMING NEUTRINOS AND ANTI-NEUTRINOS ACROSS THE EARTH TO DISENTANGLE NEUTRINO MIXING PARAMETERS
AU :	FARGION (Daniele); D'ARMIENTO (Daniele); DESIATI (Paolo); PAGGI (Paolo)
AF :	Physics Department, Rome University 1, P.le A Moro 5/00185 Rome/Italie (1 aut., 2 aut., 4 aut.); INFN Sezione di Roma, Roma 1/00185, Roma/Italie (1 aut.); Department of Physics, University of Wisconsin-Madison, 1150 University Avenue Madison/WI 53706/Etats-Unis (3 aut.)
DT :	Publication en série; Niveau analytique
SO :	The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2012; Vol. 758; No. 1 p. 1; 3.1-3.15; Bibl. 1/4 p.
LA :	Anglais
EA :	A result from MINOS seemed to indicate that the mass splitting and mixing angle of anti-neutrinos is different from that of neutrinos, suggesting a charge-parity-time (CPT) violation in the lepton sector. However, more recent MINOS data reduced the ν_μ-ν_μ differences leading to a narrow discrepancy nearly compatible with no CPT violation. However, the last few years of OPERA activity on the appearance of a tau lepton (one unique event) still has not been probed and more tools may be required to disentangle a list of parameters (μ-τ flavor mixing, tau appearance, any eventual CPT violation, θ₁₃ angle value, and any hierarchy neutrino mass). Atmospheric anisotropy in muon neutrino spectra in the DeepCore, at ten to tens of GeV (unpublished), can hardly reveal asymmetry in the eventual ν_μ-ν_μ oscillation parameters. Here we considered how the longest baseline neutrino oscillation available, crossing most of Earth's diameter, may improve the measurement and at best disentangle any hypothetical CPT violation occurring between the earliest (2010) and the present (2012) MINOS bounds (with 6σ a year), while testing τ and even the appearance of τ at the highest rate. The ν_μ and ν_μ disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of ν_μ and ν_μ crossing through the Earth, within an OPERA-like experiment from CERN (or Fermilab), in the direction of the IceCube-DeepCore ν detector at the South Pole. The ideal energy lies at 21 GeV to test the disappearance or (for any tiny CPT violation) the partial ν_μ appearance. Such a tuned detection experiment may lead to a strong signature of τ or τ generation even within its neutral current noise background events: nearly one τ or two τ a day. The tau appearance signal is above (or within) 10σ a year, even for a 1% OPERA-like experiment. Peculiar configurations for θ₁₃ and the hierarchy neutrino mass test may also be better addressed by a DeepCore-PINGU array detector beaming ν_μ and observing ν_e at 6 GeV neutrino energy windows.
CC :	001E03
FD :	Neutrino muonique; Mélangeage; Violation parité; Invariance CPT; Lepton tau; Flaveur; Hiérarchie; Masse neutrino; Anisotropie; Asymétrie; Oscillation neutrino; Diamètre; CERN; Courant neutre; Matrice détecteur; Rayonnement cosmique; Nucléosynthèse; Abondance; Particule sans masse; Masse particule élémentaire; Particule élémentaire
ED :	Muon neutrinos; Mixing; Parity violation; CPT invariance; Tau leptons; Flavor; Hierarchy; Neutrino mass; Anisotropy; Asymmetry; Neutrino oscillations; Diameter; CERN; Neutral currents; Dectector arrays; Cosmic radiation; Nucleosynthesis; Abundance; Massless particles; Elementary particle mass; Elementary particles
SD :	Violación paridad; Jerarquía; Diámetro
LO :	INIST-512.354000509554840030
ID :	12-0410344

Links to Exploration step

Pascal:12-0410344

Le document en format XML

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<front><div type="abstract" xml:lang="en">A result from MINOS seemed to indicate that the mass splitting and mixing angle of anti-neutrinos is different from that of neutrinos, suggesting a charge-parity-time (CPT) violation in the lepton sector. However, more recent MINOS data reduced the ν<sub>μ</sub>
-ν<sub>μ</sub>
 differences leading to a narrow discrepancy nearly compatible with no CPT violation. However, the last few years of OPERA activity on the appearance of a tau lepton (one unique event) still has not been probed and more tools may be required to disentangle a list of parameters (μ-τ flavor mixing, tau appearance, any eventual CPT violation, θ<sub>13</sub>
 angle value, and any hierarchy neutrino mass). Atmospheric anisotropy in muon neutrino spectra in the DeepCore, at ten to tens of GeV (unpublished), can hardly reveal asymmetry in the eventual ν<sub>μ</sub>
-ν<sub>μ</sub>
 oscillation parameters. Here we considered how the longest baseline neutrino oscillation available, crossing most of Earth's diameter, may improve the measurement and at best disentangle any hypothetical CPT violation occurring between the earliest (2010) and the present (2012) MINOS bounds (with 6σ a year), while testing τ and even the appearance of τ at the highest rate. The ν<sub>μ</sub>
 and ν<sub>μ</sub>
 disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of ν<sub>μ</sub>
 and ν<sub>μ</sub>
 crossing through the Earth, within an OPERA-like experiment from CERN (or Fermilab), in the direction of the IceCube-DeepCore ν detector at the South Pole. The ideal energy lies at 21 GeV to test the disappearance or (for any tiny CPT violation) the partial ν<sub>μ</sub>
 appearance. Such a tuned detection experiment may lead to a strong signature of τ or τ generation even within its neutral current noise background events: nearly one τ or two τ a day. The tau appearance signal is above (or within) 10σ a year, even for a 1% OPERA-like experiment. Peculiar configurations for θ<sub>13</sub>
 and the hierarchy neutrino mass test may also be better addressed by a DeepCore-PINGU array detector beaming ν<sub>μ</sub>
 and observing ν<sub>e</sub>
 at 6 GeV neutrino energy windows.</div>
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<s2>512</s2>
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<fA44><s0>0000</s0>
<s1>© 2012 INIST-CNRS. All rights reserved.</s1>
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<fA45><s0>1/4 p.</s0>
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<fA47 i1="01" i2="1"><s0>12-0410344</s0>
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<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
</fA61>
<fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0>
</fA64>
<fA66 i1="01"><s0>GBR</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>A result from MINOS seemed to indicate that the mass splitting and mixing angle of anti-neutrinos is different from that of neutrinos, suggesting a charge-parity-time (CPT) violation in the lepton sector. However, more recent MINOS data reduced the ν<sub>μ</sub>
-ν<sub>μ</sub>
 differences leading to a narrow discrepancy nearly compatible with no CPT violation. However, the last few years of OPERA activity on the appearance of a tau lepton (one unique event) still has not been probed and more tools may be required to disentangle a list of parameters (μ-τ flavor mixing, tau appearance, any eventual CPT violation, θ<sub>13</sub>
 angle value, and any hierarchy neutrino mass). Atmospheric anisotropy in muon neutrino spectra in the DeepCore, at ten to tens of GeV (unpublished), can hardly reveal asymmetry in the eventual ν<sub>μ</sub>
-ν<sub>μ</sub>
 oscillation parameters. Here we considered how the longest baseline neutrino oscillation available, crossing most of Earth's diameter, may improve the measurement and at best disentangle any hypothetical CPT violation occurring between the earliest (2010) and the present (2012) MINOS bounds (with 6σ a year), while testing τ and even the appearance of τ at the highest rate. The ν<sub>μ</sub>
 and ν<sub>μ</sub>
 disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of ν<sub>μ</sub>
 and ν<sub>μ</sub>
 crossing through the Earth, within an OPERA-like experiment from CERN (or Fermilab), in the direction of the IceCube-DeepCore ν detector at the South Pole. The ideal energy lies at 21 GeV to test the disappearance or (for any tiny CPT violation) the partial ν<sub>μ</sub>
 appearance. Such a tuned detection experiment may lead to a strong signature of τ or τ generation even within its neutral current noise background events: nearly one τ or two τ a day. The tau appearance signal is above (or within) 10σ a year, even for a 1% OPERA-like experiment. Peculiar configurations for θ<sub>13</sub>
 and the hierarchy neutrino mass test may also be better addressed by a DeepCore-PINGU array detector beaming ν<sub>μ</sub>
 and observing ν<sub>e</sub>
 at 6 GeV neutrino energy windows.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Neutrino muonique</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Muon neutrinos</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="3" l="FRE"><s0>Mélangeage</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="3" l="ENG"><s0>Mixing</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE"><s0>Violation parité</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG"><s0>Parity violation</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA"><s0>Violación paridad</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE"><s0>Invariance CPT</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG"><s0>CPT invariance</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Lepton tau</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Tau leptons</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Flaveur</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Flavor</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Hiérarchie</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Hierarchy</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Jerarquía</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Masse neutrino</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Neutrino mass</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Anisotropie</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Anisotropy</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Asymétrie</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Asymmetry</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Oscillation neutrino</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Neutrino oscillations</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="X" l="FRE"><s0>Diamètre</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="ENG"><s0>Diameter</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="SPA"><s0>Diámetro</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="3" l="FRE"><s0>CERN</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="3" l="ENG"><s0>CERN</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="3" l="FRE"><s0>Courant neutre</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="3" l="ENG"><s0>Neutral currents</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="3" l="FRE"><s0>Matrice détecteur</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="3" l="ENG"><s0>Dectector arrays</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="3" l="FRE"><s0>Rayonnement cosmique</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="3" l="ENG"><s0>Cosmic radiation</s0>
<s5>41</s5>
</fC03>
<fC03 i1="17" i2="3" l="FRE"><s0>Nucléosynthèse</s0>
<s5>42</s5>
</fC03>
<fC03 i1="17" i2="3" l="ENG"><s0>Nucleosynthesis</s0>
<s5>42</s5>
</fC03>
<fC03 i1="18" i2="3" l="FRE"><s0>Abondance</s0>
<s5>43</s5>
</fC03>
<fC03 i1="18" i2="3" l="ENG"><s0>Abundance</s0>
<s5>43</s5>
</fC03>
<fC03 i1="19" i2="3" l="FRE"><s0>Particule sans masse</s0>
<s5>44</s5>
</fC03>
<fC03 i1="19" i2="3" l="ENG"><s0>Massless particles</s0>
<s5>44</s5>
</fC03>
<fC03 i1="20" i2="3" l="FRE"><s0>Masse particule élémentaire</s0>
<s5>45</s5>
</fC03>
<fC03 i1="20" i2="3" l="ENG"><s0>Elementary particle mass</s0>
<s5>45</s5>
</fC03>
<fC03 i1="21" i2="3" l="FRE"><s0>Particule élémentaire</s0>
<s5>46</s5>
</fC03>
<fC03 i1="21" i2="3" l="ENG"><s0>Elementary particles</s0>
<s5>46</s5>
</fC03>
<fN21><s1>317</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 12-0410344 INIST</NO>
<ET>BEAMING NEUTRINOS AND ANTI-NEUTRINOS ACROSS THE EARTH TO DISENTANGLE NEUTRINO MIXING PARAMETERS</ET>
<AU>FARGION (Daniele); D'ARMIENTO (Daniele); DESIATI (Paolo); PAGGI (Paolo)</AU>
<AF>Physics Department, Rome University 1, P.le A Moro 5/00185 Rome/Italie (1 aut., 2 aut., 4 aut.); INFN Sezione di Roma, Roma 1/00185, Roma/Italie (1 aut.); Department of Physics, University of Wisconsin-Madison, 1150 University Avenue Madison/WI 53706/Etats-Unis (3 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2012; Vol. 758; No. 1 p. 1; 3.1-3.15; Bibl. 1/4 p.</SO>
<LA>Anglais</LA>
<EA>A result from MINOS seemed to indicate that the mass splitting and mixing angle of anti-neutrinos is different from that of neutrinos, suggesting a charge-parity-time (CPT) violation in the lepton sector. However, more recent MINOS data reduced the ν<sub>μ</sub>
-ν<sub>μ</sub>
 differences leading to a narrow discrepancy nearly compatible with no CPT violation. However, the last few years of OPERA activity on the appearance of a tau lepton (one unique event) still has not been probed and more tools may be required to disentangle a list of parameters (μ-τ flavor mixing, tau appearance, any eventual CPT violation, θ<sub>13</sub>
 angle value, and any hierarchy neutrino mass). Atmospheric anisotropy in muon neutrino spectra in the DeepCore, at ten to tens of GeV (unpublished), can hardly reveal asymmetry in the eventual ν<sub>μ</sub>
-ν<sub>μ</sub>
 oscillation parameters. Here we considered how the longest baseline neutrino oscillation available, crossing most of Earth's diameter, may improve the measurement and at best disentangle any hypothetical CPT violation occurring between the earliest (2010) and the present (2012) MINOS bounds (with 6σ a year), while testing τ and even the appearance of τ at the highest rate. The ν<sub>μ</sub>
 and ν<sub>μ</sub>
 disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of ν<sub>μ</sub>
 and ν<sub>μ</sub>
 crossing through the Earth, within an OPERA-like experiment from CERN (or Fermilab), in the direction of the IceCube-DeepCore ν detector at the South Pole. The ideal energy lies at 21 GeV to test the disappearance or (for any tiny CPT violation) the partial ν<sub>μ</sub>
 appearance. Such a tuned detection experiment may lead to a strong signature of τ or τ generation even within its neutral current noise background events: nearly one τ or two τ a day. The tau appearance signal is above (or within) 10σ a year, even for a 1% OPERA-like experiment. Peculiar configurations for θ<sub>13</sub>
 and the hierarchy neutrino mass test may also be better addressed by a DeepCore-PINGU array detector beaming ν<sub>μ</sub>
 and observing ν<sub>e</sub>
 at 6 GeV neutrino energy windows.</EA>
<CC>001E03</CC>
<FD>Neutrino muonique; Mélangeage; Violation parité; Invariance CPT; Lepton tau; Flaveur; Hiérarchie; Masse neutrino; Anisotropie; Asymétrie; Oscillation neutrino; Diamètre; CERN; Courant neutre; Matrice détecteur; Rayonnement cosmique; Nucléosynthèse; Abondance; Particule sans masse; Masse particule élémentaire; Particule élémentaire</FD>
<ED>Muon neutrinos; Mixing; Parity violation; CPT invariance; Tau leptons; Flavor; Hierarchy; Neutrino mass; Anisotropy; Asymmetry; Neutrino oscillations; Diameter; CERN; Neutral currents; Dectector arrays; Cosmic radiation; Nucleosynthesis; Abundance; Massless particles; Elementary particle mass; Elementary particles</ED>
<SD>Violación paridad; Jerarquía; Diámetro</SD>
<LO>INIST-512.354000509554840030</LO>
<ID>12-0410344</ID>
</server>
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BEAMING NEUTRINOS AND ANTI-NEUTRINOS ACROSS THE EARTH TO DISENTANGLE NEUTRINO MIXING PARAMETERS

BEAMING NEUTRINOS AND ANTI-NEUTRINOS ACROSS THE EARTH TO DISENTANGLE NEUTRINO MIXING PARAMETERS

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