Photospheric Magnetic Fields of the Trailing Sunspots in Active Region NOAA 12396

TL;DR

This study combines high-resolution spectropolarimetric and synoptic observations to analyze the magnetic fields of sunspots in active region NOAA 12396, providing insights into sunspot evolution and magnetic field structures.

Contribution

It presents a comprehensive analysis of sunspot magnetic fields using combined high-resolution and synoptic data, which is novel in studying sunspot growth and decay processes.

Findings

Detailed magnetic field measurements of trailing sunspots.

Insights into sunspot growth and decay mechanisms.

Correlation between photospheric and chromospheric magnetic features.

Abstract

The solar magnetic field is responsible for all aspects of solar activity. Sunspots are the main manifestation of the ensuing solar activity. Combining high-resolution and synoptic observations has the ambition to provide a comprehensive description of the sunspot growth and decay processes. Active region NOAA 12396 emerged on 2015 August 3 and was observed three days later with the 1.5-meter GREGOR solar telescope on 2015 August 6. High-resolution spectropolarimetric data from the GREGOR Infrared Spectrograph (GRIS) are obtained in the photospheric Si I $\lambda$ 1082.7 nm and Ca I $\lambda$1083.9 nm lines, together with the chromospheric He I $\lambda$1083.0 nm triplet. These near-infrared spectropolarimetric observations were complemented by synoptic line-of-sight magnetograms and continuum images of the Helioseismic and Magnetic Imager (HMI) and EUV images of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO).