Interpretation of coronal synoptic observations

Details Interpretation of coronal synoptic observations Interpretation of coronal synoptic observations

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986sfcp.nasa..257m&link_type=abstract

In NASA. Marshall Space Flight Center Solar Flares and Coronal Physics Using P/OF as a Research Tool p 257-261 (SEE N86-24614

Physics

Density Distribution, Solar Corona, Synoptic Measurement, Brightness, Coronagraphs, Eclipses, Polarized Light

Scientific paper

Three-dimensional reconstruction techniques used to determine coronal density distributions from synoptic data are complicated and time consuming to employ. Current techniques also assume time invariant structures and thus mix both temporal and spatial variations present in the coronal data. The observed distribution of polarized brightness, pB, and brightness, B, of coronal features observed either at eclipses or with coronagraphs depends upon both the three-dimensional distribution of electron density within the structure and the location of the feature with respect to the plane-of-the-sky. By theoretically studying the signature of various coronal structures as they would appear during a limb transit, it is possible to recognize these patterns in real synoptic data as well as estimate temporal evolutionary effects.

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