soho/eit, stereo-a, and sdo/aia view for solar coronal differential rotation

Differential rotation of the solar corona is challenging due to the nature of short-wavelength emissions. in this study, we aim to measure coronal differential rotation from different perspectives using observations from soho/eit at 195 å, stereo-a/euvi at 195 å, and sdo/aia at 193 å on june 1st, 2010. to achieve this, we apply a method based on zernike moments and support vector machine (svm) to identify and track coronal bright points (cbps) over a 10 hour observation period. in the heliographic coordinate system, we determine the angular velocity of the corona by fitting a linear time-dependent function to the central meridian distance of each cbp. by analyzing a collection of cbps in the solar equatorial central region (within ±50º in longitude and latitude) from each perspective, we obtain the equatorial rotation rate (a) and the latitudinal rotation gradient (b). the results indicate values of 14.32, 14.54, and 14.51 ºday-1 with -2.93, -4.03, and -3.16 ºday-1 for soho, stereo-a, and sdo, respectively.