  The 76 frequencies determined from Kepler measurements of the A-type star KIC
9700322 can be understood in a rather simple way as the radial fundamental and
first overtone radial modes, a nonradial \ell = 2 quintuplet, stellar rotation
and combinations of all of these. Two low-frequency peaks are found: f=0.160
c/d and a 2f peak. We show from a variety of arguments that the low-frequency
peak, f, (rather than the 2f peak) is the rotational frequency. The
corresponding prediction of slow rotation is confirmed by a spectrum from which
v sin i = 19 \pm 1 km/s is obtained. During rotation, the brightness changes by
0.5 ppt (parts-per-thousand, peak-to-peak). The rotation also modulates the
amplitudes of the two radial modes, leading to a small (but definite) variation
in amplitude of 0.5% of their average values. Both the rotational brightness
variations and the pulsation amplitudes form a double wave during rotation. The
variations are in phase. The maximum pulsation amplitude occurs at the
rotational phase with minimum brightness. Consequently, the 'normal' star KIC
9700322 behaves such as an extremely weak chemically peculiar star. Since such
variations are also seen in some other A stars studied by Kepler, normal stars
with a symmetric surface may not exist. The significance of this star is that
even a simple, slowly rotating, radial pulsator already shows rotational
brightness variations and modulation of the pulsation amplitude.
