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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.
Neutrinos that are created in the Sun’s core are barely absorbed, so a large quantity of them escape from the Sun and reach the Earth. Neutrinos can also offer a very strong pointing direction compared to charged particle cosmic rays. Neutrinos are very hard to detect due to their non-interactive nature.
Solar neutrinos are produced in the core of the Sun through various nuclear fusion reactions, each of which occurs at a particular rate and leads to its own spectrum of neutrino energies. Details of the more prominent of these reactions are described below. Solar neutrinos (proton–proton chain) in the standard solar model
Most people realize our Sun is producing light and heat from the fusion of hydrogen into helium. Typically, there are two processes by which smaller stars create fusion. The first of these, the ...
nuclei produced in the Sun are born in the CNO cycle. The CNO-I process was independently proposed by Carl von Weizsäcker [5] [6] and Hans Bethe [7] [8] in the late 1930s. The first reports of the experimental detection of the neutrinos produced by the CNO cycle in the Sun were published in 2020 by the BOREXINO collaboration. This was also the ...
Neutrinos were hypothesized in 1930 by Wolfgang Pauli. The first detection of antineutrinos generated in a nuclear reactor was confirmed in 1956. [2] The idea of studying geologically produced neutrinos to infer Earth's composition has been around since at least mid-1960s. [3]
Supernova neutrinos are weakly interactive elementary particles produced during a core-collapse supernova explosion. [1] A massive star collapses at the end of its life, emitting on the order of 10 58 neutrinos and antineutrinos in all lepton flavors. [2] The luminosity of different neutrino and antineutrino species are roughly the same. [3]
However, the neutrinos released by the pep reaction are far more energetic: while neutrinos produced in the first step of the p–p reaction range in energy up to 0.42 MeV, the pep reaction produces sharp-energy-line neutrinos of 1.44 MeV. Detection of solar neutrinos from this reaction were reported by the Borexino collaboration in 2012. [16]