The Solar Neutrino Problem

A few years ago Fowler (1972) published a paper in which he proposed two ‘desperate explanations’ for the solar neutrino problem. Desperation continues to be characteristic of the subject, for, in spite of many investigations over recent years, there is still no unambiguously successful model satisfying all the observational features of the Sun and giving a predicted neutrino count rate below the Davis (1972) experimental limit.

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The Solar Neutrino Problem Revisited

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000016453 ◽

1981 ◽

Vol 4 (2) ◽

pp. 227-230 ◽

Cited By ~ 2

Author(s):

J. Lattanzio

Keyword(s):

Solar Neutrino ◽

The Sun ◽

Solar Neutrino Problem

The discrepancy between the observed and predicted flux of neutrinos from the Sun is well known. Past attempts at reconciling this difference have been unconvincing (Kuchowicz 1976, Rood 1978), and hence investigations in this area continue.

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Solar Neutrino Projects

International Astronomical Union Colloquium ◽

10.1017/s0252921100067919 ◽

1990 ◽

Vol 121 ◽

pp. 157-169

Author(s):

M. Spiro ◽

D. Vignaud

Keyword(s):

Heavy Water ◽

Solar Neutrino ◽

Neutrino Oscillations ◽

Neutrino Flux ◽

The Sun ◽

Solar Neutrino Problem ◽

Wide Range ◽

Different Sources

AbstractAn overview of the solar neutrino projects is given, with an emphasis on the complementarity of the different experiments (gallium, indium, heavy water,...) to solve the solar neutrino problem that was raised by the chlorine and the Kamiokande results. The separation of the different sources of neutrinos in the Sun would contribute significantly to the astrophysical understanding of the Sun. Some of the planned experiments could be able to pinpoint neutrino oscillations (within a wide range of parameters) almost independently of solar models. Projects which are particularly sensitive to a variation of the neutrino flux with time are also discussed.

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Solar Neutrino Problem

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000013679 ◽

1973 ◽

Vol 2 (4) ◽

pp. 226-227 ◽

Cited By ~ 1

Author(s):

A. J. R. Prentice

Keyword(s):

Solar Neutrino ◽

The Sun ◽

Solar Neutrino Problem ◽

Predicted Values

A major crisis facing theoretical nuclear astronomers and physicists today is the apparently very low flux of neutrinos emitted by the Sun. Davis et al. report a measurement of 1.5 ± 1 s.n.u. (1 s.n.u. = 10−36 capture/Cl37/sec) which is a factor of 6 or so smaller than the theoretically predicted values. Numerous suggestions, often quite bizarre, have been made to account for the low flux, but so far no convincing explanation has been offered – see Fowler.

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ON THE COHERENCE CONDITION FOR RESONANT SPIN-FLAVOR PRECESSION OF MAJORANA SOLAR NEUTRINOS

International Journal of Modern Physics A ◽

10.1142/s0217751x92000569 ◽

1992 ◽

Vol 07 (06) ◽

pp. 1309-1314

Author(s):

RAUL HORVAT

Keyword(s):

Solar Neutrino ◽

Neutrino Flux ◽

Majorana Neutrino ◽

Solar Neutrinos ◽

Sunspot Activity ◽

The Sun ◽

Solar Neutrino Problem ◽

Mass Eigenstates ◽

Flavor Changing ◽

Solar Neutrino Flux

One of the most attractive solutions to the solar-neutrino problem (including an anticorrelation of the solar-neutrino flux with sunspot activity) incorporates a Majorana neutrino having a flavor-changing transition moment as large as (0.1–1)×10−10 Bohr magnetons. This solution is compatible with all known laboratory, astrophysical and cosmological bounds. Here we show the consistency of the solution with the coherence condition for effective-mass eigenstates inside the sun.

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Brief Review of Solar Models and Solar Neutrino Experiments

International Astronomical Union Colloquium ◽

10.1017/s0252921100017589 ◽

1993 ◽

Vol 137 ◽

pp. 100-107

Author(s):

Douglas R.O. Morrison

Keyword(s):

Solar Neutrino ◽

Input Data ◽

New Physics ◽

Solar Neutrinos ◽

High Variability ◽

Neutrino Masses ◽

The Sun ◽

Evolutionary Models ◽

Solar Neutrino Problem ◽

Neutrino Experiments

AbstractSolar Evolutionary Models are briefly reviewed and while the models are robust, there are uncertainties in the input data which justify rather larger errors. The 1992 experimental results from GALLEX, SAGE II and Kamiokande are shown to be consistent with calculated fluxes of solar neutrinos whereas the Chlorine results continue to be significantly low though this experiment has a problem with the high variability with time of its results in contradiction to Kamiokande. It is concluded that the evidence for a solar neutrino problem is not compelling and New Physics are not demanded. Further experiments are essential to search for neutrino masses and to study the Sun.

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PARTICLE PHYSICS CONFRONTS THE SOLAR NEUTRINO PROBLEM

International Journal of Modern Physics A ◽

10.1142/s0217751x92002465 ◽

1992 ◽

Vol 07 (22) ◽

pp. 5387-5459 ◽

Cited By ~ 45

Author(s):

PALASH B. PAL

Keyword(s):

Magnetic Moment ◽

Time Variation ◽

Solar Neutrino ◽

Particle Physics ◽

Magnetic Moments ◽

Neutrino Flux ◽

The Sun ◽

Solar Neutrino Problem ◽

The Earth ◽

Near Future

This review has four parts. In Part I, we describe the reactions that produce neutrinos in the sun and the expected flux of those neutrinos on the earth. We then discuss the detection of these neutrinos, and how the results obtained differ from the theoretical expectations, leading to what is known as the solar neutrino problem. In Part II, we show how neutrino oscillations can provide a solution to the solar neutrino problem. This includes vacuum oscillations, as well as matter enhanced oscillations. In Part III, we discuss the possibility of time variation of the neutrino flux and how a magnetic moment of the neutrino can explain the phenomenon. We also discuss particle physics models which can give rise to the required values of magnetic moments. In Part IV, we present some concluding remarks and outlook for the near future.

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The Internal Structure of the Sun and Solar Type Stars

Symposium - International Astronomical Union ◽

10.1017/s007418090000838x ◽

1976 ◽

Vol 71 ◽

pp. 453-466 ◽

Cited By ~ 2

Author(s):

IAN W. Roxburgh

Keyword(s):

Internal Structure ◽

Solar Neutrino ◽

Convective Zone ◽

The Sun ◽

Solar Oscillations ◽

Solar Constant ◽

Solar Neutrino Problem ◽

Solar Type

Our understanding of the internal structure of the Sun and solar type stars has been undermined by recent observations. In this paper we consider some of the puzzles and possible resolutions; the solar neutrino problem, lithium and beryllium abundance, rotation and calcium emission, variation of the solar constant, solar oscillations and the solar convective zone. The picture that emerges is one of confusion, and so it should be since we have no idea of what is going on inside the Sun and a fortiori of what is going on inside other stars.

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