The chromospheric component of coronal bright points. Coronal and chromospheric responses to magnetic-flux emergence

Madjarska, Maria S.; Chae, Jongchul; Moreno-Insertis, Fernando; Hou, Zhenyong; Nóbrega-Siverio, Daniel; Kwak, Hannah; Galsgaard, Klaus; Cho, Kyuhyoun
Referencia bibliográfica

Astronomy and Astrophysics

Fecha de publicación:
2
2021
Descripción
Context. We investigate the chromospheric counterpart of small-scale coronal loops constituting a coronal bright point (CBP) and its response to a photospheric magnetic-flux increase accompanied by co-temporal CBP heating.
Aims: The aim of this study is to simultaneously investigate the chromospheric and coronal layers associated with a CBP, and in so doing, provide further understanding on the heating of plasmas confined in small-scale loops.
Methods: We used co-observations from the Atmospheric Imaging Assembly and Helioseismic Magnetic Imager on board the Solar Dynamics Observatory, together with data from the Fast Imaging Solar Spectrograph taken in the Hα and Ca II 8542.1 Å lines. We also employed both linear force-free and potential field extrapolation models to investigate the magnetic topology of the CBP loops and the overlying corona, respectively. We used a new multi-layer spectral inversion technique to derive the temporal variations of the temperature of the Hα loops (HLs).
Results: We find that the counterpart of the CBP, as seen at chromospheric temperatures, is composed of a bundle of dark elongated features named in this work Hα loops, which constitute an integral part of the CBP loop magnetic structure. An increase in the photospheric magnetic flux due to flux emergence is accompanied by a rise of the coronal emission of the CBP loops, that is a heating episode. We also observe enhanced chromospheric activity associated with the occurrence of new HLs and mottles. While the coronal emission and magnetic flux increases appear to be co-temporal, the response of the Hα counterpart of the CBP occurs with a small delay of less than 3 min. A sharp temperature increase is found in one of the HLs and in one of the CBP footpoints estimated at 46% and 55% with respect to the pre-event values, also starting with a delay of less than 3 min following the coronal heating episode. The low-lying CBP loop structure remains non-potential for the entire observing period. The magnetic topological analysis of the overlying corona reveals the presence of a coronal null point at the beginning and towards the end of the heating episode.
Conclusions: The delay in the response of the chromospheric counterpart of the CBP suggests that the heating may have occurred at coronal heights.

Movies are available at http://https://www.aanda.org
Proyectos relacionados
Example of state of the art 3-D simulation of the Sun
El proyecto Whole Sun: desentrañando los complejos mecanismos físicos detrás de nuestra estrella eruptiva y sus gemelos

El Sol es una estrella activa magnéticamente cuyas erupciones violentas pueden impactar y deformar la magnetosfera terrestre y causar perturbaciones importantes en instalaciones tecnológicas en tierra y en órbita. The Whole Sun tiene como objetivo central abordar, de forma coherente y por primera vez, cuestiones actuales clave en Física Solar

Fernando
Moreno Insertis