Impact of a magnetic field distribution with multiple components on the theoretical profiles of the magnetically sensitive lines Fe I 15648.5 Å (this study) and Fe I 5497.5 Å (Kochukhov et al. 2020) for a star with solar parameters rotating with a v sin i of 5 km s⁻¹. In this case, the magnetic field distribution is composed of 0, 1, and 3 kG fields covering 75%, 20%, and 5% of the stellar surface, respectively. Top: non-magnetic spectra (blue dashed line) and combined magnetic spectra (red line). Bottom: difference between the magnetic and non-magnetic spectra (red line). The contribution to this difference by the 1 and 3 kG field is shown with the blue dashed line and black dashed line, respectively.