The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance

DOI: 
10.3847/1538-4357/ac37be
Publication date: 
01/02/2022
Main author: 
Gošić M.
IAA authors: 
Gošić, M.;Bellot Rubio, L. R.;Orozco Suárez, D.;Del Toro Iniesta, J. C.
Authors: 
Gošić, M.;Bellot Rubio, L. R.;Cheung, M. C.M.;Orozco Suárez, D.;Katsukawa, Y.;Del Toro Iniesta, J. C.
Journal: 
Astrophysical Journal
Publication type: 
Article
Volume: 
925.0
Pages: 
188
Number: 
188
Abstract: 
Small-scale internetwork (IN) magnetic fields are considered to be the main building blocks of quiet Sun magnetism. For this reason, it is crucial to understand how they appear on the solar surface. Here, we employ a high-resolution, high-sensitivity, long-duration Hinode/NFI magnetogram sequence to analyze the appearance modes and spatiotemporal evolution of individual IN magnetic elements inside a supergranular cell at the disk center. From identification of flux patches and magnetofrictional simulations, we show that there are two distinct populations of IN flux concentrations: unipolar and bipolar features. Bipolar features tend to be bigger and stronger than unipolar features. They also live longer and carry more flux per feature. Both types of flux concentrations appear uniformly over the solar surface. However, we argue that bipolar features truly represent the emergence of new flux on the solar surface, while unipolar features seem to be formed by the coalescence of background flux. Magnetic bipoles appear at a faster rate than unipolar features (68 as opposed to 55 Mx cm-2 day-1), and provide about 70% of the total instantaneous IN flux detected in the interior of the supergranule.
Database: 
SCOPUS
ADS
URL: 
https://ui.adsabs.harvard.edu/#abs/2022ApJ...925..188G/abstract
ADS Bibcode: 
2022ApJ...925..188G