English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Microflares are small dynamic signatures observed in X-ray andextreme-ultraviolet channels. Because of their impulsive emission enhancementsand wide distribution, they are thought to be closely related to coronalheating. By using the high resolution 171 {\AA} images from the AtmosphericImaging Assembly and the lines-of-sight magnetograms obtained by theHelioseismic and Magnetic Imager on board the Solar Dynamics Observatory, wetrace 10794 microflares in a quiet region near the disk center with a field ofview of 960 arcsec $\times$ 1068 arcsec during 24 hr. The microflares have anoccurrence rate of 4.4 $\times$ 10$^{3}$ hr$^{-1}$ extrapolated over the wholeSun. Their average brightness, size, and lifetime are 1.7 I$_{0}$(of the quietSun), 9.6 Mm$^{2}$, and 3.6 min, respectively. There exists a mutual positivecorrelation between the microflares' brightness, area and lifetime. In general,the microflares distribute uniformly across the solar disk, but form networkpatterns locally, which are similar to and matched with the magnetic networkstructures. Typical cases show that the microflares prefer to occur in magneticcancellation regions of network boundaries. We roughly calculate the upperlimit of energy flux supplied by the microflares and find that the result isstill a factor of $\sim$15 below the coronal heating requirement.

Relationship between EUV microflares and small-scale magnetic fields in the quiet Sun