eROSITA spectra of Her X-1 obtained during the first and the second sky surveys (left and right panels, respectively). The solid black line shows the best-fit model (see Table 1), and the green dashed line shows the contribution from the proper emission of hot photoionized plasma (not detected in the first survey). Thin red and blue lines show the blackbody and power-law components, respectively. The bottom panels show the ratio of the data to the folded model. The visible excess in the residuals at higher energies is due to the Fe K complex and possible reflection from the cold photosphere of the optical star, which are unaccounted for in the spectral modeling (see Sect. 5).