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The power spectra of the fluctuation noise of the solar active region (AR)areas and magnetic fluxes sequentially observed in time contain informationabout their geometrical features and the related fundamental physicalprocesses. These spectra are analysed for five different ARs with variousmagnetic field structures. The goal of this work is to detect thecharacteristic properties of the Fourier and wavelet spectra evaluated for thetime series of the fluctuating areas and radial magnetic fluxes of the activeregions. Accordingly, this work gathers information on the properties of noisein the different cases considered. The AR area and radial magnetic flux timeseries were built using SHARP magnetogram datasets that cover nearly the entiretime of the ARs' transits over the solar disk. Then we applied Fourier andwavelet analyses to these time series using apodization and detrendizationmethods for the cross-comparison of the results. These methods allow for thedetection and removal of the artefact data edge effects. Finally, we used alinear least-squares fitting method for the obtained spectra on a logarithmicscale to evaluate the power-law slopes of the fluctuation spectral power versusfrequency (if any). According to our results, the fluctuation spectra of theareas and radial magnetic fluxes of the considered ARs differ from each otherto a certain extent, both in terms of the values of the spectral power-lawexponents and their frequency bands. The characteristic properties of thefluctuation spectra for the compact, dispersed, and mixed-type ARs exhibitnoticeable discrepancies amongst each other. It is plausible to conclude thatthis difference might be related to distinct physical mechanisms responsiblefor the vibrations of the AR areas and/or radial magnetic fluxes.

Wide-band fluctuations of solar active regions probed with SHARP magnetograms