Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot
corona. A comprehensive understanding of solar prominences ultimately requires complex …

Eruptions, flares, and coronal mass ejection (CMEs) are due to physical phenomena mainly
driven by an initially force-free current-carrying magnetic field. We review some key …

We intend to provide a comprehensive answer to the question on whether all Coronal Mass
Ejections (CMEs) have flux rope structure. To achieve this, we present a synthesis of the …

Magnetic flux ropes play a central role in the physics of coronal mass ejections (CMEs).
Although a flux-rope topology is inferred for the majority of coronagraphic observations of …

We present a statistical study of prominence and filament eruptions observed by the
Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) …

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 …

We study an active-region dextral filament that was composed of two branches separated in
height by about 13 Mm, as inferred from three-dimensional reconstruction by combining …

Context. Prominences in the solar atmosphere represent an intriguing and delicate balance
of forces and thermodynamics in an evolving magnetic topology. How this relatively cool …

Abstract The X8. 2 event of 2017 September 10 provides unique observations to study the
genesis, magnetic morphology, and impulsive dynamics of a very fast coronal mass ejection …

We examine the three-dimensional magnetic structure and dynamics of a solar EUV-
macrospicule jet that occurred on 2011 February 27 in an on-disk coronal hole. The …