Relating Emission to Magnetic Field Evolution in Eruptive Phenomena
Abstract
The magnetohydrodynamic (MHD) equations are frequently used to investigate coronal mass ejections (CMEs), eruptive prominences, and solar flares. The proposed mechanisms responsible for these phenomena are under still under vigorous debate. Because most MHD models use relatively simple energy equations, the debate between theorists often centers on the interpretation and comparison of magnetic field evolution in the models with corresponding features observed in emission. On the other hand, observers often look at emission images and try to deduce what magnetic evolution is occurring.
We have developed MHD models that include energy transport (radiative losses, anisotropic thermal conduction, and coronal heating) in the transition region and solar corona. This more accurate representation of energy flow allows us to compute simulated EUV and X-ray emission and compare directly with observations. In this paper we will show examples of this modeling approach for specific CME events and describe the magnetic field evolution associated with commonly observed emission features such as dimming regions and postflare loops. Work supported by NASA, AFOSR, and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).- Publication:
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AAS/Solar Physics Division Meeting #40
- Pub Date:
- May 2009
- Bibcode:
- 2009SPD....40.2203L