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Title: HEATING OF THE PARTIALLY IONIZED SOLAR CHROMOSPHERE BY WAVES IN MAGNETIC STRUCTURES

In this paper, we show a “proof of concept” of the heating mechanism of the solar chromosphere due to wave dissipation caused by the effects of partial ionization. Numerical modeling of non-linear wave propagation in a magnetic flux tube, embedded in the solar atmosphere, is performed by solving a system of single-fluid quasi-MHD equations, which take into account the ambipolar term from the generalized Ohm’s law. It is shown that perturbations caused by magnetic waves can be effectively dissipated due to ambipolar diffusion. The energy input by this mechanism is continuous and shown to be more efficient than dissipation of static currents, ultimately leading to chromospheric temperature increase in magnetic structures.
Authors:
;  [1] ; ;  [2]
  1. Department of Mathematics and Information Sciences, Northumbria University, Newcastle upon Tyne, NE1 8ST (United Kingdom)
  2. Instituto de Astrofísica de Canarias, E-38205, C/Vía Láctea, s/n, La Laguna, Tenerife (Spain)
Publication Date:
OSTI Identifier:
22518609
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 819; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; AMBIPOLAR DIFFUSION; CHROMOSPHERE; DISTURBANCES; MAGNETIC FIELDS; MAGNETIC FLUX; MAGNETOHYDRODYNAMICS; NONLINEAR PROBLEMS; OSCILLATIONS; SUN; WAVE PROPAGATION