Context. Large-amplitude oscillations are a common occurrence in solar prominences.
These oscillations are triggered by energetic phenomena such as jets and flares. On March …

Context. Multidimensional solar flare simulations have not yet included a detailed analysis of
the lower atmospheric responses, such as downflowing chromospheric compressions and …

We present a study of energetic-electron trap** and acceleration in the Kelvin–Helmholtz-
induced magnetohydrodynamic (MHD) turbulence of post-flare loops in the solar corona …

During solar flares, spectral lines formed in the photosphere have been shown to exhibit
changes to their profiles despite the challenges of energy transfer to these depths. Recent …

The hour-long, gradual phase of solar flares is well observed across the electromagnetic
spectrum, demonstrating many multiphase aspects, where cold condensations form within …

The formation of the MFRs in the pre-flare stage, and how this leads to coronal rain in a post-
eruption magnetic loop is not fully understood. We explore the formation, and eruption of …

Context. Erupting magnetic flux ropes play an important role in producing solar flares,
whereas fine-scale condensed coronal rain is often found in post-flare loops. However, the …

Solar flare events are triggered by the process of magnetic reconnection, which leads to a
sudden release of stored magnetic energy and intensifies the electromagnetic emissions …

During quiescent periods on the Sun, the Lyman continuum (< 911.2 Å) forms at the base of
the transition region, the interface between the chromosphere and the corona. Therefore, the …