  We calculate and provide analytic fits of the factors which describe the
reduction of the neutrino emissivity of modified Urca and nucleon-nucleon
bremsstrahlung processes by superfluidity of neutrons and protons in
neutron-star cores. We consider $^1$S$_0$ pairing of protons and either
$^1$S$_0$ or $^3$P$_2$ pairing of neutrons. We analyze two types of $^3$P$_2$
pairing: the familiar pairing with zero projection of the total angular
momentum of neutron pairs onto quantization axis, $m_J=0$; and the pairing with
$|m_J|=2$ which leads to the gap with nodes at the neutron Fermi surface.
Combining the new data with those available in the literature we fully describe
neutrino emission by nucleons from neutron star cores to be used in simulations
of cooling of superfluid neutron stars.
