Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 819, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/2041-8205/819/1/L11
Keywords
Sun: chromosphere; Sun: magnetic fields; Sun: oscillations
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Funding
- Spanish Ministry of Science [AYA2010-18029, AYA2011-24808, AYA2014-55078-P]
- FP7 European Research Council Magnetic connectivity through the Solar Partially Ionized Atmosphere [277829]
- SOLARNET project
- European Commission's FP7 Capacities Programme [312495]
- Australian Government
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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.
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