Examples of profiles of the fluorescent iron line at 6.4 keV from our reflection simulations. We fixed R_c–i at 1.1 R_WD and varied R_p at 1.01 R_WD (left), 1.1 R_WD (center), and 1.2 R_WD (right). In the case of R_p = 1.01 R_WD, the 6.4 keV line is dominated by the component from the WD surface because of its larger solid angle over the plasma than that of the AD. Alternatively, in the other two cases a double-horn component gradually dominates the line spectrum. The energy separation of the horns is larger in the R_p = 1.1 R_WD case because the plasma is closer to the inner edge of the AD, where the Keplerian velocity is the largest. The equivalent width of the double-horn component is larger in the case of R_p = 1.2 R_WD because the solid angle of the disk is larger. (Color online)