Observation of The Transport and Storage of Magnetic Free Energy in Active Region Rotating Sunspots and Coronal Magnetic Loops

Details Observation of The Transport and Storage of Magnetic Free Energy in Active Region Rotating Sunspots and Coronal Magnetic Loops Observation of The Transport and Storage of Magnetic Free Energy in Active Region Rotating Sunspots and Coronal Magnetic Loops

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh31b..05n&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH31B-05

Physics

7513 Coronal Mass Ejections (2101), 7519 Flares, 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

Magnetic energy can be transported from below the photosphere up into the corona through torsional oscillations within the magnetic loop structure. The magnetic energy flux can be carried up by the Poynting Flux Density in the twisted loops, which has been observed at the photosphere as rotating sunspots in movies of TRACE and SOHO/MDI images (Brown et al., 2003). Rotation in flows beneath a sunspot has also been shown for the MDI helioseimology results (Zhao et al., 2003). In the corona some of the magnetic free energy can be observed in the sigmoid structures in the soft X-ray images of Yohkoh/SXT and in the EUV twisted loop structures in the TRACE data. There appears to be sufficient energy flux through the photosphere from typical sunspots rotating at 2-3 degrees per hour to provide about 10^{31} erg per day into the corona, enough energy for a small CME. In our study of active regions that have produced X-flares since 1998, it has been found that at least 95 percent of the regions contain one or more rotating sunspots, which could supply the necessary free energy for these solar eruptions. Examples of these observations and results of the study will be presented. This work has been supported by NASA, in part under the TRACE project at LMSAL (contract NAS5-38099).

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