  The problem of solar corona heating remains one of key puzzles in
astrophysics for a few decades; but none of the proposed mechanisms can give a
definitive answer to this question. As a result, the novel scenarios are still
suggested. Here, we perform a critical consideration of the recently-proposed
mechanism for the formation of anticorrelated temperature and density profiles
due to specific features of relaxation in the strongly non-equilibrium plasmas
described by the so-called spin-type Hamiltonians (L.Casetti & S.Gupta. Eur.
Phys. J. B 87, 91, 2014; T.N.Teles et al. Phys. Rev. E 92, 020101(R), 2015). We
employ the universal property of these systems to produce the long-lived
anticorrelated temperature-density distributions and analyze their most
important qualitative features in the context of coronal plasmas. As follows
from our consideration, such anticorrelated profiles can be hardly relevant to
explanation of the temperature distribution in the quiet solar corona. However,
they might be interesting for the interpretation of the large-scale
inhomogeneity in the coronal mass ejections and the resulting solar wind.
