Synchronized Observations of Bright Points from the Solar Photosphere to Corona

TL;DR

This study uses high-resolution IRIS, AIA, and HMI observations to analyze magnetic network bright points from the solar photosphere to the corona, revealing strong correlations and magnetic coupling across atmospheric layers.

Contribution

It provides new insights into the magnetic coupling and energy transport mechanisms linking the solar photosphere, chromosphere, transition region, and corona.

Findings

High correlation between TR bright network points and coronal emissions.

Strong relationship between magnetic network features and bright points across all atmospheric levels.

Magnetic-field concentrations in network rosettes facilitate coupling between inner and outer solar atmosphere.

Abstract

One of the most important features in the solar atmosphere is magnetic network and its rela- tionship with the transition region (TR), and coronal brightness. It is important to understand how energy is transported into the corona and how it travels along the magnetic-field lines be- tween deep photosphere and chromosphere through the TR and corona. An excellent proxy for transportation is the Interface Region Imaging Spectrograph (IRIS) raster scans and imaging observations in near-ultraviolet (NUV) and far-ultraviolet (FUV) emission channels with high time-spatial resolutions. In this study, we focus on the quiet Sun as observed with IRIS. The data with high signal to noise ratio in Si IV, C II and Mg II k lines and with strong emission intensities show a high correlation in TR bright network points. The results of the IRIS intensity maps and dopplergrams are compared with those of Atmo- spheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) instruments onboard the Solar Dynamical Observatory (SDO). The average network intensity profiles show a strong correlation with AIA coronal channels. Furthermore, we applied simultaneous observations of magnetic network from HMI and found a strong relationship between the network bright points in all levels of the solar atmosphere. These features in network elements exhibited high doppler velocity regions and large mag- netic signatures. A dominative fraction of corona bright points emission, accompanied by the magnetic origins in photosphere, suggest that magnetic-field concentrations in the network rosettes could help couple between inner and outer solar atmosphere.