temperature $T_{\rm c}(\rho)$. Microscopic calculations of $T_{\rm c}(\rho)$ are extremely model dependent and give a large scatter of critical temperatures. Let us mention several general features.

Neutron pairing in the spin singlet state with zero angular momentum ($^1$S$_0$) occurs in the inner neutron star crust (for free neutrons) and dies out in the core because singlet-state nuclear attraction turns into repulsion near the crust-core interface. Neutron pairing in the core may occur in a triplet state with unit angular momentum, $^3$P$_2$ (coupled to a spin triplet state with three units of angular momentum, $^3$F$_2$). Cooper pairing of other particles in the core can occur either in a singlet state or in a triple state. Baryon superfluidity is affected by the presence of pion or kaon condensate (e.g., [@tt07] and references therein). Calculated values $T_{\rm c}(\rho)$ range from $\sim 10^8$ K to a few$\times 10^{10}$ K and vanish at supranuclear densities (where attractive pairing interaction becomes inefficient).

A special case is presented by color superconductivity [@arw98] owing to very strong pairing of unlike quarks in quark matter, where $T_{\rm c}(\rho)$ can be as high as $\sim 5 \times 10^{11}$ K.

Any baryon superfluidity reduces neutrino processes involving these baryons (Tables \[tab-nucore-slow\] 