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J. Li, B.J. LaBonte (Institute for Astronomy, University of Hawaii), L.W. Acton (Department of Physics, Montana State University)
We present a useful way to study how the solar corona varies with time. Observations by EIT and SXT are used to construct limb synoptic maps. The maps show limb emissions as functions of polar angle and time.
We identify and interpret various persistent structures such as coronal hole boundaries, polar rays, and polar plumes seen on these maps. The physical properties of these structures are discussed.An empirical 3-dimensional electron density model for the background corona will be introduced. This model was obtained through the use of a median-filtering technique on the EIT coronal images obtained during solar minimum (January through May 1996).
This work was supported by NASA grant NAG5-4941 and by a subcontract with LMSAL in support of NASA contract NAS8-40801 for YOHKOH SXT.
The author(s) of this abstract have provided an email address for comments about the abstract: jing@ifa.hawaii.edu