Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...450..805l&link_type=abstract
Astronomy and Astrophysics, Volume 450, Issue 2, May I 2006, pp.805-818
Astronomy and Astrophysics
Astrophysics
42
Magnetohydrodynamics (Mhd), Magnetic Fields, Plasmas, Sun: Atmosphere, Sun: Sunspots, Sun: Magnetic Fields
Scientific paper
We present results from 2.5D numerical simulations of the emergence of magnetic flux from the upper convection zone through the photosphere and chromosphere into the corona. Certain regions of the solar atmosphere are at sufficiently low temperatures to be only partially ionised, in particular the lower chromosphere. This leads to Cowling resistivities orders of magnitude larger than the Coulomb values, and thus to anisotropic dissipation in Ohm's law. This also leads to localised low magnetic Reynolds numbers (R_m<1). We find that the rates of emergence of magnetic field are greatly increased by the partially ionised regions of the model atmosphere, and the resultant magnetic field is more diffuse. More importantly, the only currents associated with the magnetic field to emerge into the corona are aligned with the field, and thus the newly formed coronal field is force-free.
Arber T. D.
Leake James E.
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