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Coronal heating is a big question for modern astronomy. Daily measurement of985 solar spectral irradiances (SSIs) at the spectral intervals 1-39 nm and116-2416 nm during March 1 2003 to October 28 2017 is utilized to investigatecharacteristics of solar rotation in the solar atmosphere by means of the Lomb\,-\, Scargle periodogram method to calculate their power spectra. The rotationperiod of coronal plasma is obtained to be 26.3 days, and that of the solaratmosphere at the bottom of the photosphere modulated by magnetic structures is27.5 days. Here we report for the first time that unexpectedly the coronalatmosphere is found to rotate faster than the underlying photosphere. When timeseries of SSIs are divided into different cycles, and the ascending anddescending periods of a solar cycle, rotation rate in the corona is also foundto be larger than that in the photosphere, and this actually gives hiddenevidence: it is small-scale magnetic activity that heats the corona.

Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?