Volume 657, January 2022
|Number of page(s)||12|
|Section||The Sun and the Heliosphere|
|Published online||14 January 2022|
Observational evidence for two-component distributions describing solar magnetic bright points
Universidad Nacional de Colombia, Bogotá, Colombia
2 Institute of Physics, Faculty of Science, University of South Bohemia, České Budějovice, Czech Republic
3 Computational Neurosciences, Neuromed Campus, Kepler University Hospital, Linz, Austria
4 Instituto de Astrofísica de Andalucía IAA-CSIC, Granada, Spain
5 Universidad Nacional de Colombia, Observatorio Astronómico Nacional, Bogotá, Colombia
6 University of Graz, Graz, Austria
7 Instituto de Astrofísica de Canarias, Tenerife, Spain
8 Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain
9 Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovakia
10 Leibniz – Institute for Astrophysics Potsdam, Potsdam, Germany
Accepted: 30 September 2021
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 in all moments during the solar cycle, in order to establish their contribution to the behavior of the solar atmosphere, and ultimately a plausible role within the coronal heating problem.
Aims. Characterisation of size and velocity distributions of MBPs in the solar photosphere in two different datasets of quiet Sun images acquired with high-resolution solar instruments i.e. Solar Optical Telescope SOT/Hinode and the High-resolution Fast Imager HiFI/GREGOR, in the G-band (4308 Å).
Methods. In order to detect the MBPs, an automatic segmentation and identification algorithm is used. Next, the identified features were tracked to measure their proper motions. Finally, a statistical analysis of hundreds of MBPs is 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 a Rayleigh distribution revealing again for all vector elements a two component composition.
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 resolution of GREGOR and Hinode telescopes, affecting detections and average values.
Key words: Sun: photosphere / Sun: evolution / methods: observational
© ESO 2022
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.