On the Relation Between Flow Fields and Magnetic Field Evolution in Flare Productive NOAA Active Region 10486

Details On the Relation Between Flow Fields and Magnetic Field Evolution in Flare Productive NOAA Active Region 10486 On the Relation Between Flow Fields and Magnetic Field Evolution in Flare Productive NOAA Active Region 10486

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp51c..05d&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP51C-05

Physics

Optics

7519 Flares, 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

We present high resolution observations of flow fields within solar NOAA active region 10486 before an X10 flare on October 29, 2003. From 2003 October 28 to November 4, a complex δ-sunspot located in NOAA 10486 produced dramatic flare activities in the descending phase of the solar cycle 23. The flow fields are measured by local correlation tracking (LCT) based on speckle masking white-light images, near-infrared (NIR) continuum images at 1.56 μm, and G-band images obtained with the Dunn Solar Telescope (DST) of the National Solar Observatory/Sacramento Peak (NSO/SP). NSO's newly developed high-order adaptive optics system at the DST was used to achieve diffraction-limited imaging with a high signal-to-noise ratio. The spatial resolution of the images approaches the diffraction limit of the 76 cm aperture DST of about 0.14 ″ at 527 nm. In addtion, we use longitudinal magnetograms from the Michelson Doppler Imager (MDI) on board the Solar and Heliospheric Observatory (SoHO) to study the evolution of photospheric magnetic field and its correlation with flow fields in this flare productive active region. We link strong magnetic shear and fast emergence of magnetic flux to photospheric flows, which might trigger the flares. Our result suggests that the time-series analysis of the photospheric flow fields is a critical observational diagnostic for the evolution of magnetic fields in solar active regions. This work was supported by NSF under grant ATM 03-42560, ATM 03-13591, ATM 02-36945, and MRI AST 00-79482 and by NASA under grant NAG 5-13661.

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