  In this research note we present a time-resolved study of the Balmer emission
lines of RZ Leo. From the analysis of the radial velocities we find an orbital
period of 0.07651(26) d. This is in excellent agreement with the
photometrically determined periods in quiescence and during the early stages of
superoutburst. A comparison of the recently determined superhump period gives
an excess of ~0.03, which is a typical value for an SU UMa star of this period.
