The rotational characteristics of the solar corona as revealed by the coronal Fe XIV line at 5303 A are examined. Measurements of the intensity at 5303 A observed at a radius of 1.15 solar radii between 1973 and 1985 are presented. It is found that, on average, the Fe XIV corona rotates more rigidly than do features in the photosphere or chromosphere. The observations support the theory that the Fe XIV coronal signal arises from the effects of local heating on the large-scale density structure of the corona.
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Sime et al. (1989) studied this question.