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Session 6 - Corona I.
Oral session, Friday, June 27
Ballroom A, Chair: David Alexander
Solar coronal activity is intimately connected with emerging magnetic flux. In this work we explore this connection through numerical simulation; we model the emergence of magnetic flux into the solar corona. We have previously seen emerging magnetic flux drive surge-like waves in our model ``transition'' region; here we apply a new numerical technique that can bring the fully three-dimensional problem within our reach. We use high-order Godunov (HOG) shock capturing, dynamic adaptive mesh refinement (DAMR), and boundary conditions based on the characteristic waves of MHD. HOG schemes estimate fluxes by solving the Riemann shock-tube problem across cell interfaces. We will compare the results of our HOG code to those obtained with a numerical model that uses a more conventional high-order flux limiting (Flux Corrected Transport). We plan to use our numerical models to study how sheared sub-photospheric magnetic flux erupts and interacts with the solar coronal magnetic field. We are also interested in the dynamics of photospheric material during this process. Typically the dense photospheric material drains down the legs of emerging two-dimensional arcades, but to what extent will this occur for fully three dimensional structures?
