Abstract Coronal bright points (CBPs) are sets of small-scale coronal loops, connecting opposite magnetic polarities, primarily characterized by their enhanced extreme-ultraviolet (EUV) and X-ray emission. Being ubiquitous, they thought to play an important role in heating the solar corona. We aim at characterizing barely explored chromosphere underneath CBPs, focusing on related spicular activ...

Abstract In this study, we investigate the spatial distribution of highly varying plasma composition around one largest sunspots solar cycle 24. Observations photosphere, chromosphere, and corona are brought together with magnetic field modeling sunspot in order to probe conditions that regulate degree fractionation within loop populations differing connectivities. We find that, coronal above u...

ABSTRACT Explosive phenomena are known to trigger a wealth of shocks in warm plasma environments, including the solar chromosphere and molecular clouds where medium consists both ionized neutral species. Partial ionization is critical determining behaviour shocks, since ions neutrals locally decouple, allowing for substructure exist within shock. Accurately modelling partially requires careful ...

The origin of the slow solar wind is still an open issue. It has been suggested that upflows at edge active regions (AR) can contribute to wind. Here, we compared upflow region and AR core studied how plasma properties change from chromosphere via transition corona. We limb-to-limb observations NOAA 12687 (14th - 25th Nov 2017). analysed spectroscopic data simultaneously obtained IRIS Hinode/EI...

We present the results of numerical simulations of shock wave-driven jets in the solar atmosphere. The dependence of observable quantities like maximum velocity and deceleration on parameters such as the period and amplitude of initial disturbances and the inclination of the magnetic field is investigated. Our simulations show excellent agreement with observations, and shed new light on the cor...