Astronomy and Astrophysics – Astronomy
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.0109t&link_type=abstract
American Astronomical Society, SPD meeting #34, #01.09; Bulletin of the American Astronomical Society, Vol. 35, p.806
Astronomy and Astrophysics
Astronomy
Scientific paper
Following the work of Ofman and Thompson (2002), we present a three-dimensional MHD simulation of the local interaction between fast magnetosonic waves and coronal active regions. In order to have a realistic simulation, in the present work the active region is modeled by an initially potential magnetic field configuration calculated from the extrapolation of photospheric magnetograms. The density is gravitationally stratified and we also include resistive dissipation in the model. We compare the main features of the simulated wave with a wave observed with the Transition Region and Coronal Explorer (TRACE). We find that many aspects of the simulation match the observations. In particular, we show how the wave's trajectory is modified, undergoing strong reflection and refraction away from the active region. We also discuss how we can use the simulations as a tool to understand the three-dimensional topology and stability of active regions, in anticipation of the STEREO mission.
Ofman Leon
Terradas Jaume
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