Statistics – Computation
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21630505h&link_type=abstract
American Astronomical Society, AAS Meeting #216, #305.05; Bulletin of the American Astronomical Society, Vol. 41, p.854
Statistics
Computation
Scientific paper
The solar chromosphere forms the all important link between the photosphere's and convection zone's excess mechanical energy and the magnetically dominated corona and the solar wind. We still do not know which modes of nonthermal energy power the chromosphere and overlying layers. We know that waves, electrical currents, and magnetic reconnection all may release substantial energy, and that non-thermal particles, resistive dissipation, and wave damping occur. Shedding light on these issues requires that one use a variety of approaches, both theoretical and observational. In this presentation we will focus on sol called `realistic' numerical modelling and on comparing the results of numerical modelling with present and upcoming observations.
To model the chromosphere with neighboring regions from the convection zone to the corona in a realistic manner a 3D radiation magnetohydrodynamic code `Bifrost' has been developend using a sixth-order finite difference compact scheme. Radiation is treated with multi-group opacities. Conduction along the magnetic field is treated implicitly using a multi-grid approach. Novel aspects of the code are the extension of the multi-group opacity method to include scattering and the treatment of the radiative exchange in strong lines in the middle and upper chromosphere. We have there used the detailed 1D radiation-hydrodynamic simulations to develop recipes that contain the essentials of the physics while keeping the computational expenses at tractable levels. Currently we are extending the code to include the effects of partial time-dependent ionization of Hydrogen and a generalized Ohm's law.
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