Structural Analysis of the Coronal Magnetic Field
Abstract
Recent developments in the analysis of the 3D magnetic field structure have given us new insights into the properties of coronal mass ejections and the solar wind. Maps of the flux-tube squashing factor Q make it possible to identify separatrix and quasi-separatrix surfaces that delimit "building blocks" of the magnetic configuration.
When combined with high resolution MHD models of active regions, this technique gives us a powerful way to relate observed features with the underlying properties of the magnetic field, and to analyze the nature and rate of 3D magnetic reconnection. On a global scale, in particular, our method reveals the intricate structure of coronal holes and localizes a possible source of the slow solar wind. We will show how we have used this method to understand the observed properties of flare ribbons, flare arcades, and EUV and X-ray dimming regions in connection with the properties of the underlying erupting flux rope. Work supported by NASA and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).- Publication:
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American Astronomical Society Meeting Abstracts #216
- Pub Date:
- May 2010
- Bibcode:
- 2010AAS...21640607T