On The Mass and Energy Loading of EUV Brightpoints

TL;DR

This paper investigates the mass and energy dynamics of EUV brightpoints in the solar atmosphere, highlighting the role of magnetoconvection-driven reconnection and magnetic topology in their visibility across different EUV passbands.

Contribution

It provides new insights into the magnetic reconnection processes and magnetic topology changes that influence EUV brightpoints' appearance and evolution.

Findings

Magnetoconvection-driven reconnection supplies mass and energy to brightpoints.

Magnetic topology changes can increase brightpoints' visibility in hotter EUV passbands.

Surrounding supergranule magnetic conditions influence brightpoints' evolution.

Abstract

We discuss the appearance of EUV brightpoints (BPs) in the analysis of long-duration observations in the He II 304 Angstrom passband of the Solar and Heliospheric Observatory (SOHO) Extreme-ultraviolet Imaging Telescope (EIT). The signature of the observed 304 Angstrom passband intensity fluctuations around the BPs suggest that the primary source of the mass and energy supplied to the magnetic structure is facilitated by relentless magnetoconvection-driven reconnection, forced by the magnetic evolution of the surrounding supergranules. Further, we observe that if the magnetic conditions in the supergranules surrounding the footpoints of the cool 304 Angstrom BPs are sufficient (large net imbalance with a magnetic field that closes beyond the boundaries of the cell it originates in) the magnetic topology comprising the BP will begin to reconnect with the overlying corona, increasing its visibility to hotter EUV passbands and possibly Soft X-Rays.