Coronal mass ejections (CMEs) are the largest-scale eruptive phenomenon in the solar
system, expanding from active region-sized nonpotential magnetic structure to a much larger …

Solar prominences are one of the most common features of the solar atmosphere. They are
found in the corona but they are one hundred times cooler and denser than the coronal …

This review article summarizes the advancement in the studies of Earth-affecting solar
transients in the last decade that encompasses most of solar cycle 24. It is a part of the effort …

The ultrafast-rotating (P rot≈ 0.44 d) fully convective single M4 dwarf V374 Peg is a well-
known laboratory for studying intense stellar activity in a stable magnetic topology. As an …

It has been revealed that the magnetic topology in the solar atmosphere displays
hemispheric preference, ie, helicity is mainly negative/positive in the northern/southern …

Context. Helicity is a fundamental property of magnetic fields, conserved in ideal MHD. In
flux rope geometry, it consists of twist and writhe helicity. Despite the common occurrence of …

Magnetic reconnection, the process whereby magnetic field lines break and then reconnect
to form a different topology, underlies critical dynamics of magnetically confined plasmas in …

The dynamics of a filament channel are observed with imaging and spectroscopic
telescopes before and during the filament eruption on 2011 January 29. The extreme …

We have tracked a slow magnetic cloud associated coronal mass ejection (CME)
continuously from its origin as a flux rope structure in the low solar corona over a four-day …

Solar filaments exhibit a range of eruptive-like dynamic activity from the full, or partial,
eruption of the filament mass and surrounding magnetic structure, as a CME, to a fully …