Physics
Scientific paper
Mar 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..108...77p&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 108, no. 1, 1987, p. 77-87.
Physics
7
Solar Corona, Solar Cycles, Solar Electrons, Solar Magnetic Field, Solar Rotation, Boundary Value Problems, Coronal Loops, Solar Limb, Solar Wind
Scientific paper
Long-lived brightness structures in the solar electron corona persist over many solar rotation periods and permit an observational determination of coronal magnetic tracer rotation as a function of latitude and height in the solar atmosphere. For observations over 1964 - 1976 spanning solar cycle 20, the author compares the latitude dependence of rotation at two heights in the corona. Time-averaged rotation rates based on three methods of analysis demonstrate that, on average, coronal differential rotation decreases with height from 1.125 to 1.5 Rs. The observed radial variation of differential rotation implies a scale height of approximately 0.7 Rs for coronal differential rotation. Model calculations for a simple MHD loop show that magnetic connections between high and low latitudes may produce the observed radial variations of magnetic tracer rotation.
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