  The possible $^{1}S_{0}$ protonic superfluidity is investigated in neutron
star matter, and the corresponding energy gap as a function of baryonic density
is calculated on the basis of BCS gap equation. We have discussed particularly
the influence of hyperon degrees of freedom on $^{1}S_{0}$ protonic
superfluidity. It is found that the appearance of hyperons leads to a slight
decrease of $^{1}S_{0}$ protonic pairing energy gap in most density range of
existing $^{1}S_{0}$ protonic superfluidity. However, when the baryonic density
$\rho_{B}>$0.377 (or 0.409) fm${^{-3}}$ for TM1 (or TMA) parameter set,
$^{1}S_{0}$ protonic pairing energy gap is significantly larger than the
corresponding values without hyperons. And the baryonic density range of
existing $^{1}S_{0}$ protonic superfluidity is widen due to the appearance of
hyperons. In our results, the hyperons not only change the EOS and bulk
properties but also change the size and baryon density range of $^{1}S_{0}$
protonic superfluidity in neutron star matter.
