Anticorrelated temperature-density profiles in the quiet solar corona and coronal mass ejections: Approach based on the spin-type Hamiltonians

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.