Magnetic Topology of the 29 October 2003 X10 Flare

1
Magnetic Topology of the 29 October 2003 X10 Flare
Angela Des Jardins1, Richard Canfield1, Dana
Longcope1, Scott Waitukaitis2 1Physics Dept.,
Montana State University 2Physics Dept.,
University of Arizona
Introduction
Observational Results
In order to improve the understanding of both
flare initiation and evolution, we take advantage
of powerful new topological methods and the high
spatial resolution of RHESSI to examine where
magnetic reconnection takes place in
flare-producing solar active regions. Up to this
time, such studies have been carried out on a
very small number of active regions.
We use the powerful X10 flare on 29 October 2003
as a test of the ability to interpret the
topological location of reconnection. We find a
relationship between the spine lines and the
temporal evolution of the HXR flare footpoints.
In this poster, we present observations
supporting the relationship and survey possible
interpretations.
Observations
Flare location near the central meridian (80,
275) provides ideal magnetogram data for our
study on the topological location of magnetic
reconnection.
Figure 10. - MDI magnetogram with RHESSI contours
of the image in Fig. 4 (50, black), symbols as
in Fig. 6, 8 and 9, and the separators connecting
nulls in the vicinity of the RHESSI HXR sources.

References
Conclusions

• A magnetic model created by MPOLE reveals the
  existence of several candidates for reconnection
  (separators).
• The separator shown in purple in Fig. 10
  coincides with the observed high energy RHESSI
  emissions.
• The spreading motions of the footpoints along
  the spine lines is fully consistent with upward
  motion of the separator.

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