Observational evidence for two-component distributions describing solar magnetic bright points
arXiv:2110.12404 · doi:10.1051/0004-6361/202141231
Abstract
Context. High-resolution observations of the solar photosphere reveal the presence of fine structures, in particular the so-called magnetic bright points (MBPs), which are small-scale features associated with strong magnetic field regions of the order of kilogauss (kG). It is especially relevant to study these magnetic elements, which are extensively detected at all moments of the solar cycle, in order to establish their contribution to the behaviour of the solar atmosphere, and ultimately a plausible role within the coronal heating problem. Aims. We aim to characterise the size and velocity distributions of MBPs in the solar photosphere in two different datasets of quiet Sun images acquired with the Solar Optical Telescope SOT/Hinode and the High-resolution Fast Imager HiFI/GREGOR, in the G-band (4308 angstroms). Methods. In order to detect the MBPs, an automatic segmentation and identification algorithm was used. Next, the identified features were tracked to measure their proper motions. 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-normal distributions that are well fitted by two different components, whereas the velocity vector components follow Gaussians, and the vector magnitude follows a Rayleigh distribution again revealing a two-component composition for all vector elements. Conclusions. The results can be interpreted as due to the presence of two different populations of MBPs in the solar photosphere, one likely related to stronger network magnetic flux elements and the other one to weaker intranetwork flux elemens. In particular, this work concludes on the effect of the different spatial resolutions of the GREGOR and Hinode telescopes, affecting detections and average values.
arXiv commentAccepted for publication in Astronomy & Astrophysics. 12 pages, 8 figures, 2 tables
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