Solar coronal loops are the building blocks of the solar corona. These dynamic structures
are shaped by the magnetic field that expands into the solar atmosphere. They can be …

The acceleration and heating of the solar wind have been studied for decades using satellite
observations and models. However, the exact mechanism that leads to solar wind heating …

Aims. The goal of the CHIANTI atomic database is to provide a set of atomic data for the
interpretation of astrophysical spectra emitted by collisionally dominated, high temperature …

Turbulent plasma motion is common in the universe and invoked in solar flares to drive
effective acceleration leading to high-energy electrons. Unresolved mass motions are …

Adopting the MPI-AMRVAC code, we present a 2.5-dimensional magnetohydrodynamic
simulation, which includes thermal conduction and radiative cooling, to investigate the …

Context. The tearing instability plays a major role in the disruption of current sheets, whereas
thermal modes can be responsible for condensation phenomena (forming prominences and …

Context. Thermal instability plays a major role in condensation phenomena in the solar
corona (eg, for coronal rain and prominence formation). In flare-relevant current sheets …

It has been established that cold plasma condensations can form in a magnetic loop subject
to localized heating of its footpoints. In this paper, we use grid-adaptive numerical …

Context. Non-gravitationally induced condensations are observed in many astrophysical
environments. In solar physics, common phenomena are coronal rain and prominences …

Context. Thermal instabilities give rise to condensations in the solar corona, and are the
most probable scenario for coronal rain and prominence formation. We revisit the original …