MHD Simulations Spanning the Convection Zone, Chromosphere, and Corona

Details MHD Simulations Spanning the Convection Zone, Chromosphere, and Corona MHD Simulations Spanning the Convection Zone, Chromosphere, and Corona

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.0407d&link_type=abstract

American Astronomical Society, SPD meeting #34, #04.07; Bulletin of the American Astronomical Society, Vol. 35, p.811

Astronomy and Astrophysics

Astronomy

Scientific paper

The dynamics associated with evolving magnetic structures in the solar atmosphere are ultimately driven by vigorous convective motions below the photosphere. There, nonlinear interactions between the flows and fields lead to the transport of energy up into the atmosphere, which is later converted to heat in the chromosphere and corona and radiated into space. To investigate such dynamics, we have constructed a self-consistent model of the sun encompassing the upper layers of the convection zone, chromosphere, transition region, and lower corona. The fully compressible magnetized fluid comprising the convective layer is dynamically coupled to the atmosphere through the magnetic field. These models allow us to investigate the dynamics associated with waves, magnetic fields, and fluid motions within the solar atmosphere.

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