Chromospheric heating and structure as determined from high resolution 3D simulations

Details Chromospheric heating and structure as determined from high resolution 3D simulations Chromospheric heating and structure as determined from high resolution 3D simulations

2010-01-10

arxiv.org/abs/1001.1546v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

6 pages, 5 figures. To appear in the proceedings of the 25th NSO Workshop "Chromospheric Structure and Dynamics. From Old Wisd

Scientific paper

We have performed 3D radiation MHD simulations extending from the convection zone to the corona covering a box 16 Mm$^3$ at 32 km spatial resolution. The simulations show very fine structure in the chromosphere with acoustic shocks interacting with the magnetic field. Magnetic flux concentrations have a temperature lower than the surroundings in the photosphere but higher in the low chromosphere. The heating is there mostly through ohmic dissipation preferentially at the edges of the flux concentrations. The magnetic field is often wound up around the flux concentrations. When acoustic waves travel up along the field this topology leads to swirling motions seen in chromospheric diagnostic lines such as the calcium infrared triplet.

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