A model independent approach to future solar neutrino experiments

Bilenky, S.M.; Giunti, C.

doi:10.1016/0927-6505(94)90026-4

Cited by 11 publications

(13 citation statements)

References 42 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The MSW solutions in Fig. 3 compare well with the most recent two-generation analyses of the solar neutrino problem [22,23,[33][34][35][36][37][38], modulo small differences due to the input data and their treatment. In particular, we have verified that, excluding the earth regeneration effect, our results become very similar to those obtained very recently by Bahcall and Krastev in [38], where the same solar model and experimental data were used as input.…”

Section: B Two-generation Msw Analysissupporting

confidence: 70%

Matter-enhanced three-flavor oscillations and the solar neutrino problem

1996

View full text Add to dashboard Cite

We present a systematic analysis of the three-flavor Mikheyev-SmirnovWolfenstein (MSW) oscillation solutions to the solar neutrino problem, in the hypothesis that the two independent neutrino square mass differences, δm 2 and m 2 , are well separated: δm 2 ≪ m 2 . At zeroth order in δm 2 /m 2 , the relevant variables for solar neutrinos are δm 2 and two mixing angles, ω and φ. We introduce new graphical representations of the parameter space (δm 2 , ω, φ), that prove useful both to analyze the properties of the electronneutrino survival probability and to present the results of the analysis of solar neutrino data. We make a detailed comparison between the theoretical predictions of the Bahcall-Pinsonneault standard solar model and the current experimental results on solar neutrino rates, and discuss thoroughly the 1 MSW solutions found by spanning the whole three-flavor space (δm 2 , ω, φ).The allowed regions can be radically different from the usual "small mixing"and "large mixing" solutions, characteristic of the usual two-generation MSW approach. We also discuss the link between these results and the independent information on neutrino masses and mixings coming from accelerator and reactor oscillation searches. PACS number(s): 26.65.+t,14.60.Pq,13.15.+g.

show abstract

Section: B Two-generation Msw Analysissupporting

confidence: 70%

Matter-enhanced three-flavor oscillations and the solar neutrino problem

1996

View full text Add to dashboard Cite

show abstract

“…( 9). Since the 14 N(p; ) 15 O reaction is the slowest process in the CNO cycle, one must also have 15 O 13 N : (10) The luminosity constraint sets upper bounds on the allowed neutrino uxes. Since somewhat di erent amounts of energy release are associated with each of the neutrino uxes, the upper bounds depend somewhat upon the neutrino branch being considered.…”

Section: The Luminosity Constraintmentioning

confidence: 99%

How well do we (and will we) know solar neutrino fluxes and oscillation parameters?

Bahcall¹,

Krastev²

1996

Phys. Rev. D

127

View full text Add to dashboard Cite

Individual neutrino fluxes are not well determined by the four operating solar neutrino experiments. Assuming neutrino oscillations occur, the pp electron neutrino flux is uncertain by a factor of 2, the 8 B flux by a factor of 5, and the 7 Be flux by a factor of 45. For matter-enhanced oscillation ͑MSW͒ solutions, the range of allowed differences of squared neutrino masses, ⌬m 2 , varies between 4ϫ10 Ϫ6 eV 2 and 1ϫ10 Ϫ4 eV 2 , while 4ϫ10 Ϫ3 рsin 2 2р1.5ϫ10 Ϫ2 or 0.5рsin 2 2р0.9. For vacuum oscillations, ⌬m 2 varies between 5ϫ10 Ϫ11 eV 2 and 1ϫ10 Ϫ10 eV 2 , while 0.7рsin 2 2р1.0. The inferred ranges of neutrino parameters depend only weakly on which standard solar model is used. Calculations of the expected results of future solar neutrino experiments ͑SuperKamiokande, SNO, BOREXINO, ICARUS, HELLAZ, and HERON͒ are used to illustrate the extent to which these experiments will restrict the range of the allowed neutrino mixing parameters. For example, the double ratio ͑observed ratio divided by standard model ratio͒ of neutral current to charged current event rates to be measured in the SNO experiment varies, at 95% confidence limit, over the range 1.0 ͑no oscillations into active neutrinos͒, 3.1 Ϫ1.3 ϩ1.8 ͑small mixing angle MSW͒, 4.4 Ϫ1.4 ϩ2.0 ͑large mixing angle MSW͒, and 5.2 Ϫ2.9 ϩ5.6 ͑vacuum oscillations͒. We present an improved formulation of the ''luminosity constraint'' and show that at 95% confidence limit, this constraint establishes the best available limits on the rate of creation of pp neutrinos in the solar interior and provides the best upper limit to the 7 Be neutrino flux. The actual rate of creation of solar neutrinos in the solar interior to the rate predicted by the standard solar model can vary ͑while holding the CNO neutrino flux constant͒ between 0.55 and 1.08 for pp neutrinos and between 0.0 and 6.35 for 7 Be neutrinos.

show abstract

“…The NC rate (15) then does not depend on the ν e survival neutrino probability P (E), and one therefore expects R N C in the case of neutrinos undergoing RSFP to coincide with that for standard neutrinos R st N C [25,16]. Notice that for µ ν < ∼ 10 −11 µ B the electromagnetic contribution to the NC neutrino-deuteron disintegration reaction (10) due to the neutrino magnetic moment is more than eight orders of magnitude smaller than the standard electroweak one [26] and so can be safely neglected.…”

Section: Solar Magnetic Field Profilesmentioning

confidence: 99%

“…Such time dependence should be manifest in the CC reaction rate and electron spectrum, but should not be observable in the NC rate provided that neutrinos are Majorana particles [25,16]. In particular, the CC signal can have an 11-year periodicity related to the solar activity cycle [23].…”

Section: Solar Magnetic Field Profilesmentioning

confidence: 99%

See 1 more Smart Citation

SNO and the neutrino magnetic moment solution of the solar neutrino problem

Akhmedov¹,

Pulido²

2000

Physics Letters B

View full text Add to dashboard Cite

Assuming that the solar neutrino deficit observed in the Homestake, SAGE, Gallex, Kamiokande and Super-Kamiokande experiments is due to the interaction of the neutrino transition magnetic moment with the solar magnetic field, we calculate the expected values of a number of observables to be measured by SNO. For three model solar magnetic field profiles that produce the best fits of the previous data we calculate the charged current event rate, the (neutral current)/(charged current) event ratio and the charged current electron spectrum as well as its first and second moments. We study the dependence of the calculated observables on the choice of the magnetic field profile and on the value of the solar hep neutrino flux. We also compare our results with those obtained assuming that the solar neutrino problem is due to neutrino oscillations in vacuum or in matter. We show that there is an overlap or partial overlap between our predictions and those found for each of the oscillation solutions (SMA, LMA, LOW and VO). Given the uncertainties in the calculations and the expected uncertainties in the experimental results, the unambiguous discrimination between the two types of solutions to the solar neutrino problem (neutrino oscillations and magnetic moments) on the basis of the average rates and electron spectrum distortions appears to be difficult. The possible time dependence of the charged current signal and spectrum distortion in the case of the magnetic moment solution therefore remains the best hope for such a discrimination. For a hybrid solution (neutrino magnetic moment plus flavour mixing) the smoking gun signature would be an observation ofν e 's from the sun.

show abstract

A model independent approach to future solar neutrino experiments

Cited by 11 publications

References 42 publications

Matter-enhanced three-flavor oscillations and the solar neutrino problem

Matter-enhanced three-flavor oscillations and the solar neutrino problem

How well do we (and will we) know solar neutrino fluxes and oscillation parameters?

SNO and the neutrino magnetic moment solution of the solar neutrino problem

Contact Info

Product

Resources

About