Continuation of the SHINE Campaign Studies: Eruption on May 13, 2005

Details Continuation of the SHINE Campaign Studies: Eruption on May 13, 2005 Continuation of the SHINE Campaign Studies: Eruption on May 13, 2005

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh13a0274y&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH13A-0274

Physics

7513 Coronal Mass Ejections (2101), 7519 Flares, 7524 Magnetic Fields, 7954 Magnetic Storms (2788), 7974 Solar Effects

Scientific paper

We will present data on a well observed eruptive flare that occurred on May 13, 2005 in NOAA AR 0759. This typical two-ribbon flare was associated with a fast CME and caused an intense geomagnetic storm (Dst < -259nT) on early May 15th. The magnetic structure of this flare, the position of the AR, flare duration, filament activation, sigmoidal appearance in Halpha and coronal images, association with a CME and coronal dimming as well as interplanetary characteristics are strikingly similar to those of the 1997 May 12 SHINE campaign event. Because the solar and heliospheric background conditions for the May 12 1997 eruption were relatively simple, this event became a key event in many collaborative campaigns such as SHINE-GEM-CEDAR, MURI, and CISM. The biggest problem is that the 1997 event was not well observed and many essential data sets are not available. Therefore, various simulations, methods, inferences and theoretical ideas which arose from this campaign study could not be satisfactory tested against observations. It is thus, essential to continue these focused event oriented studies. The recent May 13 flare was well covered by Big Bear Solar Observatory (Halpha images and vector magnetograms) as well as SOHO, TRACE, RHESSI and ACE satellites. In this presentation we will discuss the structure of the May 13, 2005 eruption and analyze the flare light curves produced by Halpha and X- ray sources. We will also present vector magnetic field data and flow maps. We will analyze the evolution of the AR magnetic field (flux emergence and cancellation; magnetic gradients; magnetic flux change) and compare them to the flare activity and interplanetary data on the associated magnetic cloud that was observed at 1AU. Finally we will discuss our findings in terms of the existing CME models and provide observational restrains to modelers.

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