  XMM-Newton was used to observe two eclipsing, magnetic cataclysmic variables,
DP Leo and WW Hor, continuously for three orbital cycles each. Both systems
were in an intermediate state of accretion. For WW Hor we also obtained optical
light curves with the XMM-Newton Optical Monitor and from ground-based
observations. Our analysis of the X-ray and optical light curves allows us to
constrain physical and geometrical parameters of the accretion regions and
derive orbital parameters and eclipse ephemerides of the systems. For WW Hor we
directly measure horizontal and vertical temperature variations in the
accretion column. From comparisons with previous observations we find that
changes in the accretion spot longitude are correlated with the accretion rate.
For DP Leo the shape of the hard X-ray light curve is not as expected for
optically thin emission, showing the importance of optical depth effects in the
post-shock region. We find that the spin period of the white dwarf is slightly
shorter than the orbital period and that the orbital period is decreasing
faster than expected for energy loss by gravitational radiation alone.
