Hydrodynamic instabilities such as Rayleigh–Taylor (RT) and Richtmyer–Meshkov (RM)
instabilities usually appear in conjunction with the Kelvin–Helmholtz (KH) instability and are …

This paper outlines the current understanding of solar flares, mainly focused on
magnetohydrodynamic (MHD) processes responsible for producing a flare. Observations …

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 …

Observations and models of solar prominences are reviewed. We focus on non-eruptive
prominences, and describe recent progress in four areas of prominence research:(1) …

This review paper outlines background information and covers recent advances made via
the analysis of spectra and images of prominence plasma and the increased sophistication …

It has been a prevailing picture that active regions on the solar surface originate from a
strong toroidal magnetic field stored in the overshoot region at the base of the solar …

Prominences are intriguing, but poorly understood, magnetic structures of the solar corona.
The dynamics of solar prominences has been the subject of a large number of studies, and …

Magnetic flux emergence from the solar convection zone into the overlying atmosphere is
the driver of a diverse range of phenomena associated with solar activity. In this article, we …

Prominences and filaments are manifestations of magnetized, levitated plasma within the
solar coronal atmosphere. Their structure is assumed to be driven by the ambient magnetic …

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