The eclipsing active binary SV Cam ( G0V/K6V , P _ { orb } =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 \degr .
The size , temperature and Emission Measure of the flare imply an electron density of \log n _ { e } ( cm ^ { -3 } ) \sim 10.6–13.3 and a magnetic field of \sim 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 ) .