Magnetic flux supplement to coronal bright points

TL;DR

This study investigates the formation and magnetic cancellation processes of coronal bright points, revealing that magnetic flux emergence, convergence, and coalescence play key roles, with magnetic activities involving weak fields contributing to BP heating.

Contribution

It provides a detailed analysis of the magnetic flux evolution and formation processes of coronal bright points using high-resolution magnetograms and EUV imaging, highlighting multiple formation mechanisms.

Findings

Flux emergence is the main process in 52 BPs formation.

Magnetic cancellation occurs in all BPs through three different mechanisms.

Weak magnetic fields are involved in BP heating activities.

Abstract

Coronal bright points (BPs) are associated with magnetic bipolar features (MBFs) and magnetic cancellation. Here, we investigate how BP-associated MBFs form and how the consequent magnetic cancellation occurs. We analyse longitudinal magnetograms from the Helioseismic and Magnetic Imager to investigate the photospheric magnetic flux evolution of 70 BPs. From images taken in the 193 A passband of the Atmospheric Imaging Assembly (AIA) we dermine that the BPs' lifetimes vary from 2.7 to 58.8 hours. The formation of the BP MBFs is found to involve three processes, namely emergence, convergence and local coalescence of the magnetic fluxes. The formation of a MBF can involve more than one of these processes. Out of the 70 cases, flux emergence is the main process of a MBF buildup of 52 BPs, mainly convergence is seen in 28, and 14 cases are associated with local coalescence. For MBFs formed by bipolar emergence, the time difference between the flux emergence and the BP appearance in the AIA 193 \AA\ passband varies from 0.1 to 3.2 hours with an average of 1.3 hours. While magnetic cancellation is found in all 70 BPs, it can occur in three different ways: (I) between a MBF and small weak magnetic features (in 33 BPs); (II) within a MBF with the two polarities moving towards each other from a large distance (34 BPs); (III) within a MBF whose two main polarities emerge in the same place simultaneously (3 BPs). While a MBF builds up the skeleton of a BP, we find that the magnetic activities responsible for the BP heating may involve small weak fields.