Three-flavor solar neutrino oscillations with terrestrial neutrino constraints

Fogli, G. L.; Lettera, G.; Lisi, E.; Marrone, A.; Palazzo, A.; Rotunno, A. M.

doi:10.1103/physrevd.66.093008

Cited by 52 publications

(86 citation statements)

References 54 publications

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“…The observed of ν e disappearance in KamLAND has confirmed the previously favored solution in the (δm 2 , θ 12 ) parameter space, often referred to as the large mixing angle (LMA) region [16] in the literature (see, e.g., [24] and references therein). Moreover, the KamLAND data have basically split this region into two allowed subregions, which we will refer to as LMA-I and LMA-II, following Ref.…”

Section: Introductionsupporting

confidence: 63%

“…Notice that, up to ∼ 3σ, the global (SK+K2K) χ 2 function is approximately parabolic in the linear variable ∆m 2 , so that one can define a one-standard-deviation error for this parameter. This feature was already argued on the basis of a graphical reduction of the official SK and K2K likelihood functions [24], and is here confirmed through a full analysis. By keeping only the first significant figure in the error estimate, a parabolic fit provides the ±1σ range ∆m 2 = (2.6 ± 0.4) × 10 −3 eV 2 .…”

Section: "Atmospheric" Neutrinossupporting

confidence: 50%

“…The KamLAND recent observation of ν e disappearance [23] confirms the current interpretation of solar neutrino data [13,16,24,30] in terms of ν e → ν µ,τ oscillations induced by neutrino mass and mixing [18,19], and restricts the corresponding parameter space (δm 2 , θ 12 ) within the so-called large mixing angle (LMA) region. In this region, globally favored by solar neutrino data, matter effects [31,32] in adiabatic regime [33,31] are expected to dominate the dynamics of flavor transitions in the Sun (see, e.g., [34]).…”

Section: Impact Of Kamland On Solar Neutrinos (A 2ν Analysis)mentioning

confidence: 48%

“…In this region, globally favored by solar neutrino data, matter effects [31,32] in adiabatic regime [33,31] are expected to dominate the dynamics of flavor transitions in the Sun (see, e.g., [34]). The KamLAND spectral data appear to exclude some significant portions of the LMA solution [23], where the predicted spectrum distortions [24] would be in conflict with observations [23].…”

Section: Impact Of Kamland On Solar Neutrinos (A 2ν Analysis)mentioning

confidence: 99%

“…In Sections 3 we analyze the first KamLAND spectral data [23] and combine them with current solar neutrino data [8,9,10,11,13,14,15,16], assuming two-flavor oscillations of active neutrinos [24], in order to determine the surviving sub-regions of the LMA solution. In the analysis we include the CHOOZ reactor data [21].…”

Section: Introductionmentioning

confidence: 99%

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Neutrino oscillations: Global analyses

Fogli¹,

Lisi²,

Marrone

et al. 2003

Nuclear Physics B - Proceedings Supplements

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We review the status of the neutrino oscillation physics (as of June 2003), with a particular emphasis on the present knowledge of the neutrino mass-mixing parameters in a three generation approach. We consider first the ν µ → ν τ flavor transitions of atmospheric neutrinos. It is found that standard oscillations provide the best description of the SK+K2K data, and that the associated mass-mixing parameters are determined at ±1σ (and N DF = 1) as: ∆m 2 = (2.6 ± 0.4) × 10 −3 eV 2 and sin 2 2θ = 1.00 +0.00 −0.05 . Such indications, presently dominated by SK, could be strengthened by further K2K data. Then we analyze the energy spectrum of reactor ν events recently observed at KamLAND and combine them with solar and terrestrial ν data. We find that the solution to the solar ν problem at large mixing angle (LMA) is basically split into two sub-regions, that we denote as LMA-I and LMA-II. The LMA-I solution, characterized by lower values of the squared neutrino mass gap, is favored by the global data fit. Finally, we briefly illustrate how prospective data from the SNO and KamLAND can increase our confidence in the occurrence of standard matter effects in the Sun, which are starting to emerge from current data.

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Section: Introductionsupporting

confidence: 63%

Section: "Atmospheric" Neutrinossupporting

confidence: 50%

Section: Impact Of Kamland On Solar Neutrinos (A 2ν Analysis)mentioning

confidence: 48%

Section: Impact Of Kamland On Solar Neutrinos (A 2ν Analysis)mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Neutrino oscillations: Global analyses

Fogli¹,

Lisi²,

Marrone

et al. 2003

Nuclear Physics B - Proceedings Supplements

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Atmospheric neutrino oscillations, θ13 and neutrino mass hierarchy

2003

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We derive predictions for the Nadir angle (θ n ) dependence of the ratio N µ /N e of the rates of the µ−like and e−like multi-GeV events measured in water-Čerenkov detectors in the case of 3-neutrino oscillations of the atmospheric ν e (ν e ) and ν µ (ν µ ), driven by one neutrino mass squared difference, |∆m 2 31 | ∼ (2.5 − 3.0) × 10 −3 eV 2 ≫ ∆m 2 21 . This ratio is particularly sensitive to the Earth matter effects in the atmospheric neutrino oscillations, and thus to the values of sin 2 θ 13 and sin 2 θ 23 , θ 13 and θ 23 being the neutrino mixing angle limited by the CHOOZ and Palo Verde experiments and that responsible for the dominant atmospheric ν µ → ν τ (ν µ →ν τ ) oscillations. It is also sensitive to the type of neutrino mass spectrum which can be with normal (∆m 2 31 > 0) or with inverted (∆m 2 31 < 0) hierarchy. We show that for sin 2 θ 13 > ∼ 0.01, sin 2 θ 23 > ∼ 0.5 and at cos θ n > ∼ 0.4, the Earth matter effects modify substantially the θ n − dependence of the ratio N µ /N e and in a way which cannot be reproduced with sin 2 θ 13 = 0 and a different value of sin 2 θ 23 . For normal hierarchy the effects can be as large as ∼ 25% for cos θ n ∼ (0.5 − 0.8), can reach ∼ 35% in the Earth core bin cos θ n ∼ (0.84 − 1.0), and might be observable. They are typically by ∼ 10% smaller in the inverted hierarchy case. An observation of the Earth matter effects in the Nadir angle distribution of the ratio N µ /N e would clearly indicate that sin 2 θ 13 > ∼ 0.01 and sin 2 θ 23 > ∼ 0.50.

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Correlated hierarchy, Dirac masses and large mixing angles

2003

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We introduce a new parametrization of the MNS lepton mixing matrix which separates the hierarchical Grand Unified relations among quarks and leptons. We argue that one large angle stems from the charged leptons, the other from the seesaw structure of the neutral lepton mass matrix. We show how two large mixing angles can arise naturally provided there are special requirements on the Dirac (∆I w = 1/2) and Majorana (∆I w = 0) masses. One possibility is a correlated hierarchy between them, the other is that the ∆I w = 0 Majorana mass has a specific texture; it is Dirac-like for two of the three families.

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Three-flavor solar neutrino oscillations with terrestrial neutrino constraints

Cited by 52 publications

References 54 publications

Neutrino oscillations: Global analyses

Neutrino oscillations: Global analyses

Atmospheric neutrino oscillations, θ13 and neutrino mass hierarchy

Correlated hierarchy, Dirac masses and large mixing angles

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