Structure and Dynamics of the Erupting Magnetic Flux in the May 12 1997 CME Event

Details Structure and Dynamics of the Erupting Magnetic Flux in the May 12 1997 CME Event Structure and Dynamics of the Erupting Magnetic Flux in the May 12 1997 CME Event

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh51c1687t&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH51C-1687

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7531] Solar Physics, Astrophysics, And Astronomy / Prominence Eruptions

Scientific paper

The identification of erupting magnetic fluxes in solar CMEs is a big challenge from both computational and theoretical points of view. We have attacked this problem by studying the May 12 1997 CME event with the help of two powerful tools: (1) Our numerical MHD model of erupting magnetic configurations; and (2) Our generalized field line mapping technique for analyzing their magnetic structure. This approach allows us to identify the building blocks of such configurations by computing all their separatrix and quasi-separatrix surfaces that serve as interfaces between such blocks. The latter include, in particular, a flare arcade and erupting magnetic flux rope, which we relate to the observed flare ribbons and EUV dimmings of the event. On the basis of this analysis, we have also estimated the magnetic fluxes associated with these blocks at several moments in time. This provides a solid basis for a very detailed comparison of our MHD model with observational data of this eruption. Such a comparison helps us to verify our model and understand the physical processes and observed peculiarities of this event in conjunction with the dynamics of the underlying magnetic structure.

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