Photospheric bright points (BPs) fast movement is more effective than the slow movement
that occurs most of the time in transmitting energy to the corona. The splitting and merging …

Magnetic bright points in the solar photosphere, visible in both continuum and G-band
images, indicate footpoints of kilogauss magnetic flux tubes extending to the corona. The …

G-band bright points (GBPs) are regarded as good manifestations of magnetic flux
concentrations. We aim to investigate the relation between the dynamic properties of GBPs …

Six high-resolution TiO-band image sequences from the New Vacuum Solar Telescope
(NVST) are used to investigate the properties of intergranular bright points (igBPs). We …

Remote brightenings often appear at the outskirts of the active regions of solar eruptive
events. Nevertheless, their origin remains to be ascertained. In this study, we report imaging …

Umbral dots (UDs) are small isolated brightening observed in sunspot umbrae. They are
usually classified into peripheral UDs (PUDs) and central UDs (CUDs) according to their …

We present a study of a mini-filament erupting in association with a circular ribbon flare
observed by NVST and SDO/AIA on 2014 March 17. The filament was located at one …

Context. Turbulent convection efficiently transports energy up to the solar photosphere, but
its multi-scale nature and dynamic properties are still not fully understood. Several works in …

Umbral dots (UDs) are small isolated brightenings observed in sunspot umbrae. They are
convective phenomena existing inside umbrae. UDs are usually divided into central UDs …

Context. The study of the dynamic properties of small-scale magnetic fields in the quiet
photosphere is important for several reasons:(i) it allows us to characterise the dynamic …