  Optical photometry, spectroscopy and XMM-Newton ultraviolet and X-ray
observations with full phase coverage are used for an in-depth study of WXLMi,
a system formerly termed as a low-accretion rate polar. We find a constant low
mass accretion rate, M_dot ~ 1.5e-13 M_sun/yr, a peculiar accretion geometry
with one spot not being accessible via Roche-lobe overflow, a low temperature
of the white dwarf, Teff < 8000 K and the secondary likely being Roche-lobe
underfilling. All this lends further support to the changed view on WXLMi and
related systems as detached binaries, i.e. magnetic post-common envelope
binaries without significant Roche-lobe overflow in the past. The transfer rate
determined here is compatible with accretion from a stellar wind. We use
cyclotron spectroscopy to determine the accretion geometry and to constrain the
plasma temperatures. Both, cyclotron spectroscopy and X-ray plasma diagnostics
reveal low plasma temperatures below 3 keV on both accretion spots. For the low
m_dot, high B plasma at the accretion spots in WXLMi, cyclotron cooling is
dominating thermal plasma radiation in the optical. Optical spectroscopy and
X-ray timing reveal atmospheric, chromospheric and coronal activity at the
saturation level on the dM4.5 secondary star.
