Physics – Plasma Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43a1938o&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH43A-1938
Physics
Plasma Physics
[7507] Solar Physics, Astrophysics, And Astronomy / Chromosphere, [7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7827] Space Plasma Physics / Kinetic And Mhd Theory, [7959] Space Weather / Models
Scientific paper
We present an improved global, 3D numerical model of the solar atmosphere and solar wind, extending from the upper chromosphere to 1AU. The model solves the magnetohydrodynamic equations coupled to a wave kinetic equation for low frequency Alfven waves. The waves accelerate the plasma through the action of wave pressure gradients, and also constitute a source of heating via wave dissipation. It is assumed that Alfven waves are launched from the chromosphere, with amplitudes that match recent observations by Hinode and SDO. In the somewhat complex magnetic topology of the sun, closed field line regions will be filled with counter propagating waves. We propose a wave dissipation mechanism that treats open and closed field line regions on the same footing, without the need to determine a priori if the field line is open or closed (e.g. via field line tracing or a potential field approximation), as was the case in our previous solar wind models. Excess of heat generated by wave dissipation can be conducted down towards the cooler chromosphere, where it can be more efficiently radiated away. The combination of Alfven wave heating, heat conduction and radiative cooling will allow us to reach a steady state solution for the solar atmosphere. We find that our dissipation mechanism can account for the observed coronal temperatures without invoking additional heating functions. The model is based on the BATSRUS code, and is developed as part of the Space Weather Modeling Framework (SWMF). Coupling the chromosphere-coronal solution to the existing Inner Heliosphere component of the SWMF allows us to compare our model results with in situ observations at 1AU.
der Holst Bart van
Gombosi Tamas I.
Oran Rona
Sokolov Iu. I.
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