Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp51a02b&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SP51A-02
Other
7519 Flares, 7524 Magnetic Fields, 7529 Photosphere
Scientific paper
With the Flare Genesis Experiment (FGE), a balloon-borne 80-cm solar telescope, we observed the active region NOAA 8844 on January 25, 2000 for several hours. FGE was equipped with a vector polarimeter and a lithium-niobate Fabry-Perot narrow-band filter. It recorded time series of filtergrams, vector magnetograms, and dopplergrams at the CaI 6122.2 Angstroms line, as well as Hα filtergrams, with a cadence between 2.5 and 7.5 minutes. At the time of the observations NOAA 8844 was located at approximately 5 deg N, 30 deg W. It was a new flux emergence that first appeared on the solar disk two days before and was still showing a very dynamic behavior. Its two main polarity parts were rapidly moving away from each other and new magnetic flux was constantly emerging from its center. Here we describe the structure and behavior of peculiar small moving magnetic dipoles (called moving magnetic features MMF's) that we observed near the trailing negative polarity sunspot of NOAA 8844. Presentations by D. M. Rust, and by M. K. Georgoulis at this meeting will focus on other aspects of the same active region. The MMF's took the form of small dipoles that first emerged into the photosphere near the center of a supergranular cell located next to the main trailing flux concentration. They rapidly migrated towards the spot, following the supergranular flow. The two polarities of the little dipoles did not separate; they moved together with same speed and in the same direction. The dipoles were oriented parallel to their motion toward the negative spot, with the positive polarity always leading. MMF's usually move away from sunspots, and their orientation is the reverse of what we see here. In addition, we noted that the dipole structure was not symmetric. The field lines of the trailing part of the MMF's (negative polarity) were always much more perpendicular to the local horizontal than the ones of the leading part. The trailing part looked more compact and circular, while the leading part was more elongated in the direction of the motion. We conclude that we observed a new type of MMF's with a totally different magnetic structure than previously seen. We present a possible model that could explain their unusual structure and behavior. This work was supported by NASA grant NAG5-8331 and NSF grant OPP-9909167.
Bernasconi Pietro N.
Georgoulis Manolis K.
LaBonte Barry J.
Rust David Maurice
Schmieder Brigitte
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