The Close Binary (CB) SV Cam has an orbital period 
.
According to Hall (1976), it belongs to the short-period group of the
RS CVn binaries. Hilditch et al. (1979) found that this system is
composed of a G3V primary, and K4V secondary, with the mass ratio
q=m2/m1=0.7. They made the hypothesis that the light variations are due
to a BY Draconis-type variability of the K4V secondary. The careful
photometry by Patkós (1982) demonstrated conclusively the existence of a
"distortion wave", which migrates toward increasing orbital phase, and strong
flaring activity, which Patkós (1981) attributed to the active regions on
the secondary star.
Using the Patkós' (1982) observations, Busso et al. (1985) analysed the differential rotation problem on the basis of the depression migration (caused by spotted areas) through the light curve orbital phase with time. By using a simplified model, the authors estimated the relevant parameters, such as the angular velocity at the equator, the differential rotation rate, the mean velocity of the meridional motion, the latitude of spots at formation and the corotation latitude.
Observations extending over about half a century (1932-1984) were analysed by
Zeilik et al. (1988) in the framework of the spot modelling technique
(Budding
1977; Budding & Zeilik 1987) with spots on the primary. According to these
authors, the active dark spotted region covers a significant part of the stellar
surface occupying high latitudes (about 
). The single active region
tends to fall into two longitude sectors, 
and 
. These
resemble the active longitude belts such as proposed by
Eaton & Hall
(1979) for the RS CVn group in general.