  Coronal heating is a big question for modern astronomy. Daily measurement of
985 solar spectral irradiances (SSIs) at the spectral intervals 1-39 nm and
116-2416 nm during March 1 2003 to October 28 2017 is utilized to investigate
characteristics of solar rotation in the solar atmosphere by means of the Lomb
\,-\, Scargle periodogram method to calculate their power spectra. The rotation
period of coronal plasma is obtained to be 26.3 days, and that of the solar
atmosphere at the bottom of the photosphere modulated by magnetic structures is
27.5 days. Here we report for the first time that unexpectedly the coronal
atmosphere is found to rotate faster than the underlying photosphere. When time
series of SSIs are divided into different cycles, and the ascending and
descending periods of a solar cycle, rotation rate in the corona is also found
to be larger than that in the photosphere, and this actually gives hidden
evidence: it is small-scale magnetic activity that heats the corona.
