Synoptic photoelectric observations of the coronal Fe XIV and Fe X emission lines at 530.3 nm and 637.4 nm, respectively, are analyzed to study the rotational behavior of the solar corona as a function of latitude, height and time. The data used are measurements made with the Sacramento Peak 40-cm coronagraph and Emission-Line Coronal Photometer of the intensity of these lines observed at 1.15 to 1.45 solar radii (R_☉) between 1973 (1984 for Fe X) and 2000. An earlier similar temporal-correlation analysis of the Fe XIV data at 1.15 R_☉ over only one 11-year solar activity cycle (Sime, Fisher, & Altrock 1989) found suggestions of solar-cycle variations in the differential-rotation and latitude-averaged-rotation patterns that combined the effects of large-scale patterns seen in the white-light corona and smaller-scale patterns seen in chromospheric and photospheric rotation. These results are tested over the longer epoch now available. In addition, the new 1.15 R_☉ Fe XIV results are compared with those at greater heights and with results from the Fe X line to form a global picture of solar rotation throughout the corona and over more than two solar cycles.
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