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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 :

RBID : Pascal:12-0410344

Descripteurs français

English descriptors

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 νμμ 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 Atmospheric anisotropy in muon neutrino spectra in the DeepCore, at ten to tens of GeV (unpublished), can hardly reveal asymmetry in the eventual νμμ oscillation parameters.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 νμ and νμ disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of νμ and νμ 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 νμ 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 νμ and observing νe at 6 GeV neutrino energy windows.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

pA  
A01 01  1    @0 0004-637X
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.
A20       @2 3.1-3.15
A21       @1 2012
A23 01      @0 ENG
A43 01      @1 INIST @2 512 @5 354000509554840030
A44       @0 0000 @1 © 2012 INIST-CNRS. All rights reserved.
A45       @0 1/4 p.
A47 01  1    @0 12-0410344
A60       @1 P
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 νμμ 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 νμμ 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 νμ and νμ disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of νμ and νμ 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 νμ 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 νμ and observing νe 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
C03 02  3  ENG  @0 Mixing @5 27
C03 03  X  FRE  @0 Violation parité @5 28
C03 03  X  ENG  @0 Parity violation @5 28
C03 03  X  SPA  @0 Violación paridad @5 28
C03 04  3  FRE  @0 Invariance CPT @5 29
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
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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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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 νμμ 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 νμμ 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 νμ and νμ disappearance correlated with the tau appearance is considered for those events at the largest distances. We thus propose a beam of νμ and νμ 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 νμ 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 νμ and observing νe 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

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Pascal:12-0410344

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<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
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<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>
<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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<sub>μ</sub>
<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>
<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>
<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>
<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>
</inist>
</record>

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