Thermodynamic MHD Modeling of Coronal Mass Ejections

Details Thermodynamic MHD Modeling of Coronal Mass Ejections Thermodynamic MHD Modeling of Coronal Mass Ejections

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.5805l&link_type=abstract

American Astronomical Society Meeting 210, #58.05; Bulletin of the American Astronomical Society, Vol. 39, p.168

Astronomy and Astrophysics

Astronomy

Scientific paper

Coronal mass ejections (CMEs) disrupt the large-scale coronal magnetic field and propel plasma and magnetic flux outward into interplanetary space. The most energetic CMEs typically originate from active regions on the Sun. Accurately modeling active regions while also capturing the entire corona requires MHD models that include energy transport (radiative losses,anisotropic thermal conduction, and coronal heating) in the transition region and solar corona. We refer to this as the thermodynamic MHD model.
The more accurate representation of energy flow in the thermodynamic MHD model allows us to to compute simulated EUV and X-ray emission as would be observed from spacecraft such as SOHO, STEREO, and Hinode. With this approach, theorists no longer get to argue what emission they think their favorite model's magnetic field evolution implies; we can actually go compute the emission and compare with observations. As an example, we show a simulation of the May 12, 1997 CME, and compare the simulated emission with observations from the actual event of dimming regions, postflare loops, and reformation of loops near the northern polar coronal hole.
Work supported by NASA, NSF and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).

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