AAS 204th Meeting, June 2004
Session 27 Magnetic Reconnection Flares and CMEs
SPD Oral, Monday, May 31, 2004, 2:00-3:30pm, 704

[Previous] | [Session 27] | [Next]

[27.01] High resolution flare observations using adaptive optics

T. Rimmele, K. Sankarasubramanian (NSO)

We present a time sequence of a flare observed on October 23, 2003 in active region NOAA 0486 near the east limb. The same active region produced the huge flare on October 29, 2003. The Universal Birefringened Filter (UBF) was used to record narrow band filtergrams in H-\alpha and the iron line FeI 5434. The Diffraction-Limited Spectro- Polarimeter (DLSP) performed vector magnetic field measurements before and after the flare. The high order adaptive optics system provided diffraction limited imaging during a large fraction of the time during which the flare was observed.

The dynamic H-\alpha core flare sequence, during which a super-penumbral loop system erupts, will be shown. We were able to resolve finestructure in the flare ribbons at scales of 0.2. Footpoints of loops as well as individual loop tops are seen to brighten as the loop system erupts. To our knowledge for the first time we observe flare structure at spatial scales of 0.2 - the diffraction limit of the DST. H-\alpha wing dopplergrams show structure on similar spatial scales. The signature of the flare is also seen in the core of the line FeI 5434 Å, which forms in the upper photosphere. Comparing DLSP vector magnetograms before and after the flare we find evidence of flux cancellation at small spatial scales.

[Previous] | [Session 27] | [Next]

Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.