Solar neutrinos and the Mikheyev-Smirnov-Wolfenstein theory

Journal Article · Fri Nov 15 00:00:00 EST 1991 · Physical Review, D (Particles Fields); (United States)

DOI:https://doi.org/10.1103/PhysRevD.44.2962· OSTI ID:6157150

Bethe, H A ^[1]; Bahcall, J N ^[2]

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1. Newman Laboratory of Nuclear Studies, Cornell University, Ithaca, New York (USA)
2. Institute for Advanced Study, Princeton, New Jersey (USA)

The observation of solar neutrinos by Kamiokande shows that the solar-neutrino problem cannot be solved by changing the solar model. In combination with the observations with a chlorine detector, it makes the nonadiabatic form of the Mikheyev-Smirnov-Wolfenstein theory most likely, and determines {Delta}{ital m}{sup 2}sin{sup 2}{theta}=1.0{times}10{sup {minus}8} eV{sup 2}. Probably all neutrinos go through the resonance in the Sun, those from {sup 8}B nonadiabatically, all others adiabatically. The latter emerge from the Sun in the higher-mass eigenstate {nu}{sub 2} and have a probability sin{sup 2}{theta} to be detected as {nu}{sub {ital e}}. The gallium experiments, when done with sufficient accuracy, will be able to determine {Delta}{ital m}{sup 2}={ital m}{sup 2}({nu}{sub {mu}}){minus}{ital m}{sup 2}({nu}{sub {ital e}}) within fairly close limits. If the day-night effect can be measured, it will further constrain these limits. The small value of {Delta}{ital m}{sup 2}sin{sup 2}{theta} explains why the oscillation from {nu}{sub {ital e}} to {nu}{sub {mu}} has not been observed in the laboratory. From existing experiments, the temperature at the center of the Sun can be determined to be within about 6% of that derived from the standard solar model; future neutrino experiments may determine it to within 1%.

• OSTI ID: 6157150
• Journal Information: Physical Review, D (Particles Fields); (United States), Vol. 44:10; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
SOLAR NEUTRINOS
MASS
CHLORINE
CROSS SECTIONS
EIGENSTATES
ELECTRON NEUTRINOS
GALLIUM
NEUTRINO DETECTION
NEUTRINO OSCILLATION
NEUTRINO-ELECTRON INTERACTIONS
PROBABILITY
RECOILS
SCATTERING
STANDARD MODEL
DETECTION
ELEMENTARY PARTICLES
ELEMENTS
FERMIONS
HALOGENS
INTERACTIONS
LEPTON-LEPTON INTERACTIONS
LEPTONS
MASSLESS PARTICLES
MATHEMATICAL MODELS
METALS
NEUTRINOS
NONMETALS
PARTICLE INTERACTIONS
PARTICLE MODELS
RADIATION DETECTION
RADIATIONS
SOLAR PARTICLES
SOLAR RADIATION
STELLAR RADIATION
UNIFIED GAUGE MODELS
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