HR: 1340h
AN: SH53A-1066    [Abstracts]
TI: Feature Tracking of Hinode Magnetograms
AU: * Lamb, D
EM: derek@boulder.swri.edu
AF: Dept of Astrophysical and Planetary Sciences, University of Colorado, 391 UCB, Boulder, CO 80309-0391, United States
AU: DeForest, C E
EM: deforest@boulder.swri.edu
AF: Dept of Space Studies, Southwest Research Institute, 1050 Walnut Street Suite 300, Boulder, CO 80302, United States
AU: Hagenaar, H J
EM: hagenaar@lmsal.com
AF: Lockheed Martin Advanced Technology Center, Org. ADBS., Bldg. 252, Palo Alto, CA 94304, United States
AU: Parnell, C E
EM: clare@mcs.st-and.ac.uk
AF: School of Mathematics and Statistics, St. Andrews University, St. Andrews, KY16 9S, United Kingdom
AU: Welsch, B T
EM: welsch@ssl.berkeley.edu
AF: University of California at Berkeley Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720-7450, United States
AB: We present results of applying feature tracking to a sequence of Hinode magnetograms. The single line wing Na D 5896 magnetograms have a high signal-to-noise ratio, allowing the detection of flux approximately 30 times weaker than in MDI magnetograms. We find evidence that, even with Hinode's improved resolution and sensitivity, we do not always detect the bipolar emergence of new magnetic flux. This suggests that we have not reached the ultimate resolution to observe the fundamental flux generation processes in the photosphere.
DE: 7524 Magnetic fields
DE: 7529 Photosphere
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting