Photospheric magnetic topology of a north polar region

Abstract

Aims. We aim to characterise the magnetism of a large fraction of the north polar region close to a maximum of activity, when the polar regions are reversing their dominant polarity. Methods. We make use of full spectropolarimetric data from the CRisp Imaging Spectro-Polarimeter installed at the Swedish Solar Telescope. The data consist of a photospheric spectral line, which is used to infer the various physical parameters of different quiet Sun regions by means of the solution of the radiative transfer equation. We focus our analysis on the properties found for the north polar region and their comparison to the same analysis applied to data taken at disc centre and low-latitude quiet Sun regions for reference. We also analyse the spatial distribution of magnetic structures throughout the north polar region. Results. We find that the physical properties of the polar region (line-of-sight velocity, magnetic flux, magnetic inclination and magnetic azimuth) are compatible with those found for the quiet Sun at disc centre and are similar to the ones found at low latitudes close to the limb. Specifically, the polar region magnetism presents no specific features. The structures for which the transformation from a line-of-sight to a local reference frame was possible harbour large magnetic fluxes ($>10^{17}$ Mx) and are in polarity imbalance with a dominant positive polarity, the largest ones ($>10^{19}$ Mx) being located below $73^{\circ }$ latitude.

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Cited by in corpus (4)

• Center-to-limb variation of spectral lines and continua observed with SST/CRISP and SST/CHROMIS
• The non-LTE formation of the Fe I 6173 A line in the solar atmosphere
• Improvement of the Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Inversion Code
• On the center-to-limb variations of the He I 10830 Å triplet