  We present an analysis of the X-ray spectra of two strongly magnetic
cataclysmic variables, DP Leo and WW Hor, made using XMM-Newton. Both systems
were in intermediate levels of accretion. Hard optically thin X-ray emission
from the shocked accreting gas was detected from both systems, while a soft
blackbody X-ray component from the heated surface was detected only in DP Leo.
We suggest that the lack of a soft X-ray component in WW Hor is due to the fact
that the accretion area is larger than in previous observations with a
resulting lower temperature for the re-processed hard X-rays. Using a
multi-temperature model of the post-shock flow, we estimate that the white
dwarf in both systems has a mass greater than 1 Msun. The implications of this
result are discussed. We demonstrate that the `soft X-ray excess' observed in
many magnetic cataclysmic variables can be partially attributed to using an
inappropriate model for the hard X-ray emission.
