Solar and atmospheric neutrino oscillations with three flavors

Narayan, Mohan; Murthy, M. V. N.; Rajasekaran, G.; Sankar, S. Uma

doi:10.1103/physrevd.53.2809

Cited by 34 publications

(51 citation statements)

References 27 publications

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“…(1), one can show that the solar neutrino problem depends only on δm 2 21 , ω and φ while the atmospheric neutrino problem depends only on δm 2 32 , ψ and φ. It is this simplification that allows us to analyse the two problems within a 3 − ν framework under reasonable control and one gets a fairly broad and stable set of allowed regions in the 5-parameter space [4,5]. If we temporarily put φ as zero, then the two problems decouple and the results are the following :-There are three solutions of the solar neutrino problem : [6] turns out to be a crucial result.…”

Section: Resultsmentioning

confidence: 99%

“…Extensive literature exists on the solar [4,10] and atmospheric neutrinos [5,11]. So, we shall be brief.…”

Section: Solar Atmospheric and Reactor Neutrinosmentioning

confidence: 99%

“…The high-quality data coming out from the great neutrino experiments of the present-day deserve to be treated by a realistic 3 − ν analysis rather than the 2 − ν toy model often used by the experimenters to give their results. This is the point of view with which we started our ν-phenomenology work at IMSc [4]. When we started, there were very few groups doing a 3 − ν analysis.…”

Section: Introductionmentioning

confidence: 99%

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Phenomenology of neutrino oscillations

Rajasekaran

2000

Pramana - J Phys

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Section: Resultsmentioning

confidence: 99%

“…Extensive literature exists on the solar [4,10] and atmospheric neutrinos [5,11]. So, we shall be brief.…”

Section: Solar Atmospheric and Reactor Neutrinosmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Phenomenology of neutrino oscillations

Rajasekaran

2000

Pramana - J Phys

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“…As before the analysis is done assuming the standard mass hierarchy necessitated by the solar and atmospheric neutrino observations [23]. We also impose all the known constraints on the mixing parameters and mass-squared differences including those constraints from laboratory experiments [21,24].…”

Section: Introductionmentioning

confidence: 99%

Neutrinos from stellar collapse: Comparison of signatures in water and heavy water detectors

et al. 2001

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Signatures of neutrino and antineutrino signals from stellar collapse in heavy water detectors are contrasted with those in water detectors. The effects of mixing, especially due to the highly dense matter in the supernova core, are studied. The mixing parameters used are those sets allowed by current understanding of available neutrino data: from solar, atmospheric and laboratory neutrino experiments. Signals at a heavy water detector, especially the dominant charged current reactions on deuteron, are very sensitive to some of these sets of allowed mixing parameters. Theoretical uncertainties on supernova neutrino spectra notwithstanding, a combination of supernova measurements with water and heavy water detectors may be able to distinguish many of these mixing possibilities and thus help in ruling out many of them.

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“…It has been shown [11,15] that the simultaneous solution of both the solar and the atmospheric neutrino problems requires the mass hierarchy δ 31 ≫ δ 21 and under this condition δ 31 also drops out. The rediagonalization of the mass matrix in the presence of matter (in the sun or earth) under the hierarchy condition leads to the following results [11] tan 2ω m = δ 21 sin 2ω where A is the Wolfenstein term A = 2 √ 2 G F N e E (N e is the number density of electrons and E is the neutrino energy) . We note that δ 31 ≫ A, for A evaluated at any point in the sun or the earth.…”

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confidence: 99%

Time-of-Night Variation of Solar Neutrinos

1998

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We investigate the time-of-night variation of solar neutrino rate which will be of relevance to SuperKamioka and Sudbury neutrino detectors in the framework of oscillations among the three flavors. An analytical method of computing the regeneration in the earth is presented. If day-night effect is seen, we show how the study of the time-of-night variation will allow the determination of the neutrino parameters.PACS number: 14.60. Pq, 95.30.Cq, 96.40.Tv, 96.60.Jw It has been known for quite some time that an asymmetry between night rate and day rate for the real time solar neutrino detectors is an unambiguous signal for neutrino mixing and oscillations. Conversely the absence of such an effect can put constraints on the neutrino masses and mixing angles. Although no day-night asymmetry outside the error-bars was seen at the Kamioka detector [1,2] the high statistics detectors like Super-Kamioka [3], SNO [4]and Borexino [5] will be much more effective in investigating this effect. If there is a day-night asymmetry, then the profile of the asymmetry as a function of the time during night is a very sensitive function of the neutrino parameters. The counting rates in these detectors are expected to be high enough for the study of this time-of-night variation. The aim of this note is to focus attention on this aspect of the day-night effect [6], in view of the fact that Super-Kamioka has already started functioning and SNO is expected to do so soon.The neutrino samples different amounts of matter in the earth during a single night and also during a year. The distance d travelled by the neutrino inside the earth during night, as a function of time t, is given byR is the radius of the earth, φ l is the latitude of the location of the detector, T D is the length of the day, T Y is the length of the year and zero of t is chosen at midnight on autumnal equinox. Thus assuming that the neutrino parameters are in a suitable range, neutrino data collected as a function of t contain an enormous amount of information on neutrino oscillations, which in principle can be analyzed to yield the neutrino parameters.The time variation of x = ( d 2R ) during the night and year are illustrated in Fig.1a. If the data collected during successive nights are accumulated at the corresponding x-bins, the calculation of neutrino rates per unit bin will require the function f (x) defined as the time duration per unit interval of x [7]. f (x) for different locations are plotted in Fig.1b, which shows the relative merits of the detectors for exposure to regions of x. We now describe an analytical method of calculating the neutrino regeneration effect in the earth. Let a neutrino of flavor α be produced at time t = t 0 in the core of the sun. Its state vector iswhere |νare the mass eigenstates with mass eigenvalues µ C i and U C αi are the elements of the mixing matrix in the core of the sun. We use Greek index α to denote the flavors e, µ,τ and Latin index i to denote the mass eigenstates i = 1,2,3. The neutrino propagates in the sun adiabatica...

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Solar and atmospheric neutrino oscillations with three flavors

Cited by 34 publications

References 27 publications

Phenomenology of neutrino oscillations

Phenomenology of neutrino oscillations

Neutrinos from stellar collapse: Comparison of signatures in water and heavy water detectors

Time-of-Night Variation of Solar Neutrinos

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