  The generalized Tsallis statistics produces a distribution function
appropriate to describe the interior solar plasma, thought as a stellar
polytrope, showing a tail depleted respect to the Maxwell-Boltzmann
distribution and reduces to zero at energies greater than about $20 \, k_{_B}
T$. The Tsallis statistics can theoretically support the distribution suggested
in the past by Clayton and collaborators, which shows also a depleted tail, to
explain the solar neutrino counting rate.
