  In magnetically accreting white dwarfs, the height above the white dwarf
surface where the standing shock is formed is intimately related with the
accretion rate and the white dwarf mass. However, it is difficult to measure.
We obtained new data with NuSTAR and Swift that, together with archival Chandra
data, allow us to constrain the height of the shock in the intermediate polar
EX Hya. We conclude that the shock has to form at least at a distance of about
one white dwarf radius from the surface in order to explain the weak Fe
K{\alpha} 6.4 keV line, the absence of a reflection hump in the high-energy
continuum, and the energy dependence of the white dwarf spin pulsed fraction.
Additionally, the NuSTAR data allowed us to measure the true, uncontaminated
hard X-ray (12-40 keV) flux, whose measurement was contaminated by the nearby
galaxy cluster Abell 3528 in non-imaging X-ray instruments.
