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Solar neutrino observations and neutrino oscillations
Physical Review D, 1990The results of recent Kamiokande-II and {sup 37}Cl solar-neutrino experiments are quantitatively analyzed assuming the Mikheyev-Smirnov-Wolfenstein solution to the solar-neutrino problem. It is found that the parameter region known as the large mass'' solution to the solar-neutrino problem is disfavored by a little more than 1 {sigma} while the small ...
, Kuo, , Pantaleone
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International Journal of Modern Physics D, 1992
Solar neutrinos have been measured by a radioactive scheme involving 37 Cl , and by electron collisions at Kamiokande II. The former experiment gave 1/4, the latter 1/2 of the intensity expected from the standard solar model. Kamiokande showed that the central temperature from the standard model is at least approximately correct.
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Solar neutrinos have been measured by a radioactive scheme involving 37 Cl , and by electron collisions at Kamiokande II. The former experiment gave 1/4, the latter 1/2 of the intensity expected from the standard solar model. Kamiokande showed that the central temperature from the standard model is at least approximately correct.
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International Journal of Modern Physics A, 1998
The current status of solar neutrino experiments is reviewed. All the experimental measurements show deficits of solar neutrinos. Non monotonic suppression indicates that the problem may naturally be explained by neutrino oscillations, but not by modifying solar models. A new experiment shows very promising results.
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The current status of solar neutrino experiments is reviewed. All the experimental measurements show deficits of solar neutrinos. Non monotonic suppression indicates that the problem may naturally be explained by neutrino oscillations, but not by modifying solar models. A new experiment shows very promising results.
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Physical Review Letters, 1985
The theory of oscillations of solar neutrinos is developed as it applies to the electron-recoil spectrum in neutrino-electron scattering. The spectral information obtained by such measurements (as opposed to counting total event rates) is crucial for allowing observation of neutrino oscillations for masses down to 500 neV.
, Krauss, , Wilczek
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The theory of oscillations of solar neutrinos is developed as it applies to the electron-recoil spectrum in neutrino-electron scattering. The spectral information obtained by such measurements (as opposed to counting total event rates) is crucial for allowing observation of neutrino oscillations for masses down to 500 neV.
, Krauss, , Wilczek
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Nuclear Instruments and Methods, 1973
The observed capture rate for solar neutrinos in the 37Cl detector is lower than the predicted capture rate. This discrepancy between theory and observation is known as the ‘solar neutrino problem’. I review the basic elements in this problem: the detector efficiency, the theory of stellar (solar) evolution, the nuclear physics of energy generation ...
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The observed capture rate for solar neutrinos in the 37Cl detector is lower than the predicted capture rate. This discrepancy between theory and observation is known as the ‘solar neutrino problem’. I review the basic elements in this problem: the detector efficiency, the theory of stellar (solar) evolution, the nuclear physics of energy generation ...
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Reviews of Modern Physics, 1978
New results are presented for absorption cross sections of nine possible detectors of solar neutrinos ($^{7}\mathrm{Li}$, $^{37}\mathrm{Cl}$, $^{51}\mathrm{V}$, $^{55}\mathrm{Mn}$, $^{71}\mathrm{Ga}$, $^{81}\mathrm{Br}$, $^{87}\mathrm{Rb}$, $^{115}\mathrm{In}$, and $^{205}\mathrm{Tl}$). Special attention is given to nuclear physics uncertainties.
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New results are presented for absorption cross sections of nine possible detectors of solar neutrinos ($^{7}\mathrm{Li}$, $^{37}\mathrm{Cl}$, $^{51}\mathrm{V}$, $^{55}\mathrm{Mn}$, $^{71}\mathrm{Ga}$, $^{81}\mathrm{Br}$, $^{87}\mathrm{Rb}$, $^{115}\mathrm{In}$, and $^{205}\mathrm{Tl}$). Special attention is given to nuclear physics uncertainties.
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Physical Review Letters, 1989
The observation of solar neutrinos at Kamiokande rules out the Mikheyev-Smirnov-Wolfenstein (MSW) theory with a large'' mass difference between the neutrinos, {Delta}{ital m}{sup 2}{congruent}10{sup {minus}4} eV{sup 2}. There remain the MSW theory with a small {Delta}{ital m}{sup 2}{congruent}10{sup {minus}7} eV{sup 2} or the assumption of unexpectedly
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The observation of solar neutrinos at Kamiokande rules out the Mikheyev-Smirnov-Wolfenstein (MSW) theory with a large'' mass difference between the neutrinos, {Delta}{ital m}{sup 2}{congruent}10{sup {minus}4} eV{sup 2}. There remain the MSW theory with a small {Delta}{ital m}{sup 2}{congruent}10{sup {minus}7} eV{sup 2} or the assumption of unexpectedly
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Neutrino Oscillations and Solar Neutrinos
Physics Today, 1989The neutrino is the elementary particle postulated by Wolfgang Pauli to account for the apparent nonconservation of energy in nuclear beta decay. Neutrinos are now believed to exist in at least three varieties, or “flavors,” labeled νe, νμ and ντ and distinguished by the way they interact. There are also three antineutrinos, ν̄e, ν̄μ and ν̄τ.
Lincoln Wolfenstein, Eugene W. Beier
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Nonaccelerator Astroparticle Physics, 2002
Neutrinos have been and are abundantly produced in the Universe and neutrino astronomy provides very rich information either in astrophysics or in particle physics. We focus in this review on neutrinos as witnesses of the life of stars (solar neutrinos) and on neutrinos as messengers of the death of stars (supernov= neutrinos).
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Neutrinos have been and are abundantly produced in the Universe and neutrino astronomy provides very rich information either in astrophysics or in particle physics. We focus in this review on neutrinos as witnesses of the life of stars (solar neutrinos) and on neutrinos as messengers of the death of stars (supernov= neutrinos).
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