Top: EW of the Fe Kα fluorescent line due to reflection on the WD surface as a function of the height of the accretion shock above the WD surface. The short-dashed cyan, solid blue, and long-dashed magenta lines correspond to the hot DA, the DO, and the moderately cool DA WD models, respectively. In all cases, an inclination of 45° was assumed. Bottom: synthetic profile for an individual component of the Fe Kα fluorescent line produced in the hot DA WD atmosphere for ${\upsilon }_{\text{rot}}^{\text{WD}}=25\text{km}{\text{s}}^{-1}$, h_s = 0.04 R_WD, i = 45°, and accretion taking place at the magnetic pole assumed to coincide with the rotational pole.