Understanding Eruptive Phenomena with Thermodynamic MHD Simulations
Abstract
Understanding Eruptive Phenomena with Thermodynamic MHD Simulations The magnetohydrodynamic (MHD) equations are frequently used to investigate coronal mass ejections, eruptive prominences, and solar flares. A key goal of such studies is to deduce how energy stored in the magnetic field is suddenly released to drive these phenomena, for which the proposed mechanism(s) is (are) under still under vigorous debate. Because most MHD models use relatively simple energy equations, the discussion often centers on the interpretation and comparison of magnetic field evolution in the models with corresponding features observed in emission. With new capabilities to study X-ray and EUV emission from Hinode, as well as complementary observations from STEREO and SOHO, it now becomes imperative that models advance to more quantitative comparisons with emission measurements. We have developed 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 approach as "Thermodynamic MHD." This more accurate representation of energy flow allows us to compute simulated EUV and X-ray emission and compare directly with observations. In this talk we will show examples of this modeling approach for specific events and describe the magnetic field evolution associated with commonly observed emission features such as dimming regions and postflare loops. Work supported by NASA and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).
- Publication:
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37th COSPAR Scientific Assembly
- Pub Date:
- 2008
- Bibcode:
- 2008cosp...37.1786L