The magnetic white dwarf WD 1953-011 demonstrates the presence of two-component magnetic field geometry in photosphere. The geometry consists of a weak, large-scale component, and a strong, localized component (magnetic ``spot''). The localized component of the field is derived from variable due to the star's rotation circular polarization and intensity spectra. The flux from WD 1953-011 is also variable with rotation in the V-band filter. This variability can be explained by the presence of a dark spot having a magnetic nature, analogous to sunspots. Motivated by this idea, and using all available observations of WD 1953-011 we examine the possible physical relationships between the suggested dark spot and the strong-field magnetic structure recently identified on the surface of this star. Comparing the rotationally-modulated flux with the variable spectral observables related to the magnetic ``spot'' we establish their physical relationship. We discuss this result in the frame of the first observational evidences for the presence of active magnetic structures in magnetic white dwarfs.