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

▪ Abstract Solar coronal mass ejections (CMEs) are a major form of activity on the Sun. A
CME takes 1015-16 g of plasma from the low corona into the solar wind, to disturb the near …

We compute the three-dimensional magnetic field of an active region in order to study the
magnetic configuration of active region filaments. The nonlinear force-free field model is …

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 …

In this paper we present a numerical study of the time evolution of solar prominences
embedded in sheared magnetic arcades. The prominence is represented by a density …

The magnetic configuration hosting prominences and their surrounding coronal structure is
a key research topic in solar physics. Recent theoretical and observational studies strongly …

The temporal evolution of a solar prominence inserted in a three-dimensional magnetic flux
rope is investigated numerically. Using the model of Titov & Démoulin under the regime of …

The new approach to the modeling of quiescent solar prominences is proposed. We solve
the inverse magnetohydrostatic problem, when the pressure, density and temperature of …

Solar magnetic flux ropes are core structures driving solar activities. We construct a
magnetic flux rope for a filament/prominence observed at 01: 11 UT on 2011 June 21 in AR …

Solar prominence models used so far in the analysis of MHD waves in two-dimensional
structures are quite elementary. In this work, we calculate numerically magnetohydrostatic …