  The eclipsing active binary SV Cam (G0V/K6V, P_0.593071 d) was observed with
XMM-Newton during two campaigns in 2001 and 2003. No eclipses in the quiescent
emission are clearly identified, but a flare was eclipsed during the 2001
campaign, allowing us to strongly constrain, from purely geometrical
considerations, the position and size of the event: the flare is compact and it
is formed at a latitude below 65 deg. The size, temperature and Emission
Measure of the flare imply an electron density of log n_e (cm^-3)~10.6-13.3 and
a magnetic field of ~65-1400 G in order to confine the plasma, consistent with
the measurements that are obtained from density-sensitive line ratios in other
similar active stars. Average emission seems to come from either extended or
polar regions because of lack of eclipses. The Emission Measure Distribution,
coronal abundances and characteristics of variability are very similar to other
active stars such as AB Dor (K1V).
