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 …

Solar cycle 23 witnessed the most complete set of observations of coronal mass ejections
(CMEs) associated with the Ground Level Enhancement (GLE) events. We present an …

As observed in Thomson-scattered white light, coronal mass ejections (CMEs) are manifest
as large-scale expulsions of plasma magnetically driven from the corona in the most …

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

We present the first unambiguous detection of quasi-periodic wave trains within the broad
pulse of a global EUV wave (so-called EIT wave) occurring on the limb. These wave trains …

Determining the 3D coronal magnetic field is a critical, but extremely difficult problem to
solve. Since different types of multiwavelength coronal data probe different aspects of the …

Magnetic flux ropes are topological structures consisting of twisted magnetic field lines that
globally wrap around an axis. The torus instability model predicts that a magnetic flux rope of …

Solar prominences are long-lived cool and dense plasma curtains in the hot and rarefied
outer solar atmosphere or corona. The physical mechanism responsible for their formation …

A clear understanding of the nature of the pre-eruptive magnetic field configurations of
Coronal Mass Ejections (CMEs) is required for understanding and eventually predicting …

Solar flares are powerful radiations occurring in the Sun's atmosphere. They are powered by
magnetic reconnection, a phenomenon that can convert magnetic energy into other forms of …