2020/02/20 by Yurii V. Dumin, Dumin, Yurii V.
Physics and Astronomy · #FOS: Physical sciences #Ionosphere and magnetosphere dynamics #Plasma Physics (physics.plasm-ph) #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.2002.08624
openalex publication_date 2020/02/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The problem of solar corona heating remains one of key puzzles in\nastrophysics for a few decades; but none of the proposed mechanisms can give a\ndefinitive answer to this question. As a result, the novel scenarios are still\nsuggested. Here, we perform a critical consideration of the recently-proposed\nmechanism for the formation of anticorrelated temperature and density profiles\ndue to specific features of relaxation in the strongly non-equilibrium plasmas\ndescribed by the so-called spin-type Hamiltonians (L.Casetti & S.Gupta. Eur.\nPhys. J. B 87, 91, 2014; T.N.Teles et al. Phys. Rev. E 92, 020101(R), 2015). We\nemploy the universal property of these systems to produce the long-lived\nanticorrelated temperature-density distributions and analyze their most\nimportant qualitative features in the context of coronal plasmas. As follows\nfrom our consideration, such anticorrelated profiles can be hardly relevant to\nexplanation of the temperature distribution in the quiet solar corona. However,\nthey might be interesting for the interpretation of the large-scale\ninhomogeneity in the coronal mass ejections and the resulting solar wind.\n