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

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