  These descriptive comments are made to encourage detailed three-body,
relativistic, quantum collision calculations for the pp reaction. In stars,
coulomb barrier tunneling, as in the pp reaction, is not a two-body process.
Tunneling is mediated by an energetic electron that interacts with the
colliding particles. The presence of such an electron lowers the potential
barrier and increases the probability of tunneling by orders of magnitude. The
solar luminosity can be maintained with a central temperature near 10 million K
where the neutrino production rates correspond to the observed rates. Current
stellar interior and evolutionary models need substantial revision.
