  The observed rapid cooling of the neutron star Cassiopeia A is usually
interpreted as being caused by transitions of neutrons and protons in the
star's core from the normal state to the superfluid and superconducting state.
However, this so-called "minimal" cooling paradigm faces the problem of
numerically simulating the observed anomalously fast drop in the neutron star
surface temperature using theoretical neutrino energy losses from superfluid
neutrons. As a solution to this problem, I propose a somewhat more complex
cooling model, in which, in addition to superfluid neutrons, direct Urca
processes from a very small central part of the neutron star core are also
involved. Numerical simulations of the cooling trajectory in this scenario show
excellent agreement with observations of the Cassiopeia A neutron star. The
proposed cooling scenario unambiguously relates the used equation of state and
the mass of the neutron star. For a neutron star constructed according to BSk25
equation of state, the most appropriate are the mass $M=1.62M_{\sun}$ and the
radius $R=12.36$ km. If BSk24 equation of state is used, then the most suitable
solution is $M=1.60M_{\sun}$ and $R=12.55$ km.
