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In the first reaction of the p-p chain, a proton decays into a neutron in the immediate
vicinity of another proton. The two particles form a heavy variety of hydrogen known as
deuterium, along with a positron and an electronneutrino. There is a second reaction in the
p-p chain producing deuterium and a neutrino by involving two protons and an electron. This
reaction (pep-reaction) is 230 times less likely to occur in the solar core than the first
reaction between two protons (pp-reaction). The deuterium nucleus produced in the pp- or
pep-reaction fuses with another proton to form helium-3 and a gamma ray. About 88% of the
time the p-p chain is completed when two helium-3 nuclei react to form an helium-4 nucleus
and two protons, which may return to the beginning of the p-p chain. However, 12% of the
time, a helium-3 nucleus fuses with a helium-4 nucleus to produce beryllium-7 and a gamma
ray. In turn the beryllium-7 nucleus absorbs an electron and transmutes into lithium-7 and
an electronneutrino. Only once for every 5000 completions of the p-p chain, beryllium-7
reacts with a proton to produce boron-8 which immediately decays into two helium-4 nuclei, a
positron and an electronneutrino.
The net result of either the p-p chain or CNO cycle is the production of helium nuclei and
minor abundances of heavier elements as 7Be,
7Li, 8Be,
8B (in the case of the p-p chain) or
13N, 14N,
15N (in the case of the CNO cycle). The energy generated by
thermonuclear reactions in the form of gamma rays is streaming (actually, diffusing) toward
the solar surface, thereby getting scattered, absorbed and reemitted by nuclei and
electrons. On their way outward, the high-energy gamma ray is progressively changed to
x-ray, to extreme ultraviolet ray, to ultraviolet ray and finally emerges mainly as visible
light from the solar surface and radiates into outer space. Only the weakly interacting
neutrinos can leave the solar core with almost no interaction with solar matter. However,
the chlorine experiment of Davis and collaborators, the Japanese Kamiokande experiment, and
the GALLEX experiment at Gran Sasso to detect solar neutrinos show that the Sun emits fewer
of these elusive particles than the standard solar model predicts (Iben 1969; Lande 1989;
Hirata et al. 1991; Anselmann et al. 1992 a,b). Since the beginning of the 70's this deficit
challenges current understanding of solar and neutrino physics and of the process by which
the Sun shines. The mystery of the missing solar neutrinos is commonly referred to as the
"solar neutrino problem" (Bahcall and Davis 1982).
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