The time dependence of the brightness at both central eclipses of the RS CVn, binary SV Cam, observed between 1973 and 1980 by Patkos (1982), is analyzed to check the activity model, which was derived from light variations outside the eclipses by Busso et al. (1984). Their detection of a cycle of about 10 years is confirmed by observations of the primary eclipses, whereas from observations of the secondary eclipses an un-ambiguous determination of a cycle length was not possible. Obviously, the cycle is superimposed with fluctuating short-term variations which exist in time scales from days up to months. These fluctuations are observed not only at the primary eclipse but also at the secondary eclipse. Correlations between the fluctuations at these two orbital phases suggest the primary component of SV Cam to be the main contributor to the variations observed.