  We model X-ray reflection from white dwarfs (WD) in magnetic cataclysmic
variables (mCVs) with a Monte Carlo simulation. A point source with a power-law
spectrum or a realistic post-shock accretion column (PSAC) source irradiates a
cool and spherical WD. The PSAC source emits thermal spectra of various
temperatures stratified along the column according to the PSAC model. In the
point source simulation, we confirm (1) a source harder and nearer to the WD
enhances the reflection, (2) higher iron abundance enhances the equivalent
widths (EWs) of fluorescent iron K${\alpha}_{1,2}$ lines and their Compton
shoulder, and increases cut-off energy of a Compton hump, and (3) significant
reflection appears from an area that is more than 90 deg apart from the
position right under the point X-ray source because of the WD curvature. The
PSAC simulation reveals that (1) a more massive WD basically enhances the
intensities of the fluorescent iron K${\alpha}_{1,2}$ lines and the Compton
hump, except for some specific accretion rate, because the more massive WD
makes the hotter PSAC from which higher energy X-rays are preferentially
emitted, (2) a larger specific accretion rate monotonically enhances the
reflection because it makes the hotter and shorter PSAC, and (3) the intrinsic
thermal component hardens by occultation of the cool base of the PSAC by the
WD. We quantitatively evaluate influences of the parameters on the EWs and the
Compton hump with both types of sources. We also calculate X-ray modulation
profiles brought about by the WD spin. They depend on angles of the spin axis
from the line of sight and from the PSAC, and whether the two PSACs can be
seen. The reflection spectral model and the modulation model involve the
fluorescent lines and the Compton hump and can directly be compared to the data
which allow us to evaluate these geometrical parameters with unprecedented
accuracy.
