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AIA 171A AR 11131 12/08/10
 
Inroduction and Overview
 
 
     Data Sets: These data files contain a set of coronal loop mappings, created by Hassan Robert Liaghati-Mobaran, UAH undergraduate physics major, in the 2011-2012 year, using JHelioviewr data sets and a Mathematica program written by Dr. G. Allen Gary/CSPAR/NSSTC/UAHuntsville. The Bezier coefficients of the set of closed and open coronal loops are in the files BezierDataMDROpen.tex and BezierDataMDRClosed.txt Included in the data sets are the images from Solar Dynamis Observatory specral filters 171,193,211,304,355,1600, and 1700 Angstroms and the Helioseismic and Magnetic Imager (HMI) line-of-site magnetogram images. The AIA instrument home web site address is http://aia.lmsal.com/index.htm and the HMI instrument home web site address is http://hmi.stanford.edu/. The major advantages of using Bezier curves to map the coronal features are- (1) they provide a method to change the shape of the curve with only a few paramters in order to match a coronal loop, (2) the variation of the simple parameters change the shape of the curve in a predictable manner, (3) the curve automatically starts and ends at the user defined foot points: and (4) the curves and their derivatives with respect to a parameter, exits and can be determined in an analytic form. Furthermore, for a closed loop the end Bezier control points are the end points of the loop. The principal investigator is Dr Qiang Hu, Asst. Professor at Physics/CSPAR/UAHuntsville, for this study under the National Science Foundation SHINE grant AGS-1062050 entitled "Analysis of Solar Active Region Energetics Based on Non-Force-Free Coronal Magnetic Field Extrapolation".

Disclaimer: "Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation."
 
 
 
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