Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43a1924p&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH43A-1924
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7959] Space Weather / Models
Scientific paper
One of the key challenges in constructing magnetohydrodynamic (MHD) models capable of capturing solar coronal dynamics on a global scale, is to realistically model the acceleration and expansion of the solar wind. However, the physical processes responsible for heating the solar corona and accelerating the solar wind remain unknown. To circumvent this, various pragmatic ad-hoc heating schemes are often applied. In this work, we demonstrate by performing MHD simulations of erupting coronal mass ejections (CMEs) on identical steady-state solar wind solutions obtained using different heating schemes, that the properties of the CME driven shock are significantly altered depending on the heating scheme. Thus, for simulations where capturing the shock physics is essential, the effect of the applied heating scheme should be carefully assessed. As a remedy, we propose a simple heating function formulation suitable for such MHD simulations.
Pomoell Jens
Vainio Rami O.
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