Ad
related to: solar neutrino probability density function
Search results
Results From The WOW.Com Content Network
Theoretical curves of survival probability of solar neutrinos that arrive on day (orange, continuous) or on night (purple, dashed), as a function of the energy of the neutrinos. Also shown the four values of the energy of the neutrinos at which measurements have been performed, corresponding to four different branches of the proton–proton chain.
The solar neutrino problem concerned a large discrepancy between the flux of solar neutrinos as predicted from the Sun's luminosity and as measured directly. The discrepancy was first observed in the mid-1960s and was resolved around 2002.
This was dramatically confirmed in the Sudbury Neutrino Observatory (SNO), which has resolved the solar neutrino problem. SNO measured the flux of solar electron neutrinos to be ~34% of the total neutrino flux (the electron neutrino flux measured via the charged current reaction, and the total flux via the neutral current reaction). The SNO ...
A neutrino (/ nj uː ˈ t r iː n oʊ / new-TREE-noh; denoted by the Greek letter ν) is an elementary particle that interacts via the weak interaction and gravity. [2] [3] The neutrino is so named because it is electrically neutral and because its rest mass is so small that it was long thought to be zero.
Neutrino oscillation is a function of the ratio L / E , where L is the distance traveled and E is the neutrino's energy. (Details in § Propagation and interference below.) All available neutrino sources produce a range of energies, and oscillation is measured at a fixed distance for neutrinos of varying energy.
The interaction probability will depend on the number of nucleons the neutrino passed along its path, which is directly related to density. If the initial flux is known (as it is in the case of atmospheric neutrinos), then detecting the final flux provides information about the interactions that occurred.
Therefore, in their main statistical analyses, the OPERA group generated a model of the proton waveforms at CERN, took the various waveforms together, and plotted the chance of neutrinos being emitted at various times (the global probability density function of the neutrino emission times). They then compared this plot against a plot of the ...
However, another solar model from around the same time gives only 7.14 percent of neutrinos from the later steps and 92.86 percent from the synthesis of deuterium nuclei. [10] The difference is apparently due to slightly different assumptions about the composition and metallicity of the sun. There is also the extremely rare p–p IV branch ...