Strong solar flares and coronal mass ejections, here defined not only as the bursts of
electromagnetic radiation but as the entire process in which magnetic energy is released …

Magnetic fields play a fundamental role in the structure and dynamics of the solar corona. As
they are driven by their footpoint motions on the solar surface, which transport energy from …

Magnetic reconnection is a multi-faceted process of energy conversion in astrophysical,
space and laboratory plasmas that operates at microscopic scales but has macroscopic …

Abstract The Solar Upper Transition Region Imager (SUTRI) onboard the Space Advanced
Technology demonstration satellite (SATech-01), which was launched to a Sun …

The solar corona is two to three orders of magnitude hotter than the underlying photosphere,
and the energy loss of coronal plasma is extremely strong, requiring a heating flux of over …

Coronal mass ejections (CMEs) and solar flares are the large-scale and most energetic
eruptive phenomena in our solar system and able to release a large quantity of plasma and …

Magnetic flux ropes are characterized by coherently twisted magnetic field lines, which are
ubiquitous in magnetized plasmas. As the core structure of various eruptive phenomena in …

Solar filaments are an intriguing phenomenon, like cool clouds suspended in the hot corona.
Similar structures exist in the intergalactic medium as well. Despite being a long-studied …

Magnetoseismology, a technique of magnetic field diagnostics based on observations of
magnetohydrodynamic (MHD) waves, has been widely used to estimate the field strengths …

We present a clear case study on the occurrence of two successive X-class flares, including
a decade-class flare (X9. 3) and two coronal mass ejections (CMEs) triggered by shearing …