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Context. High-resolution observations of the solar photosphere reveal thepresence of fine structures, in particular the so-called magnetic bright points(MBPs), which are small-scale features associated with strong magnetic fieldregions of the order of kilogauss (kG). It is especially relevant to studythese magnetic elements, which are extensively detected at all moments of thesolar cycle, in order to establish their contribution to the behaviour of thesolar atmosphere, and ultimately a plausible role within the coronal heatingproblem. Aims. We aim to characterise the size and velocity distributions ofMBPs in the solar photosphere in two different datasets of quiet Sun imagesacquired with the Solar Optical Telescope SOT/Hinode and the High-resolutionFast Imager HiFI/GREGOR, in the G-band (4308 angstroms). Methods. In order todetect the MBPs, an automatic segmentation and identification algorithm wasused. Next, the identified features were tracked to measure their propermotions. Finally, a statistical analysis of hundreds of MBPs was carried out,generating histograms for areas, diameters, and horizontal velocities. Results.This work establishes that areas and diameters of MBPs display log-normaldistributions that are well fitted by two different components, whereas thevelocity vector components follow Gaussians, and the vector magnitude follows aRayleigh distribution again revealing a two-component composition for allvector elements. Conclusions. The results can be interpreted as due to thepresence of two different populations of MBPs in the solar photosphere, onelikely related to stronger network magnetic flux elements and the other one toweaker intranetwork flux elemens. In particular, this work concludes on theeffect of the different spatial resolutions of the GREGOR and Hinodetelescopes, affecting detections and average values.

Observational evidence for two-component distributions describing solar magnetic bright points