A crucial step for understanding the origin of the high temperatures in the upper atmosphere is an accurate description of the energy transport. Current studies on the energy flux in the solar atmosphere mainly focus on the vertical electromagnetic flow through the photosphere, ignoring the possible Poynting flux’s contributions to local heating. This study used observational data from Sunrise/IMaX and Bifrost simulations to analyse the electromagnetic energy flux of the lower atmosphere. Based on a simulated quiet Sun atmosphere, we found that only a small fraction of the Poynting energy flows upwards in the photosphere. See more at https://espos.stream/2022/06/09/Silva/.

NASA’s Sounding Rocket Program has provided essential contributions to space science since 1959 and has proved to be one of the most robust, versatile, and cost-effective flight programs at NASA. On the 29th May 2018, the High-resolution Coronal Imager (Hi-C) was launched for a third time from the White Sands Missile Range, NM, USA capturing 329 seconds of 17.2 nm data of target active region AR 12712, with a cadence of ~4s and a plate scale of ~0.129 arcsec. This unique dataset provides some of the highest-resolution EUV observations of coronal loops to date. In this presentation, the spatial scales of these fundamental building blocks of the solar corona are explored and the results from Hi-C are discussed with respect to SDO/AIA and Solar Orbiter.

Space weather forecasting is a complex problem which involves modeling of the solar plasma all the way from the solar corona down to the Earth’s atmosphere. To simulate this energy transfer, a cascade of various models is required, such as the coronal model, the heliospheric model and various models to estimate the Kp and Dst indices. European efforts to create such a framework of connected tools have resulted in the launch of the Virtual Space Weather Modeling Center (VSWMC) (Poedts et al., 2019) - a platform we will briefly introduce in the beginning of this talk. Read further at https://espos.stream/2022/10/20/Brchnelova/.

Spicular jets are highly elongated chromospheric plasma features that are believed to transport momentum to the solar wind and non-thermal energy to heat the atmosphere. At any given time, it is estimated that about 3 million spicules are present on the Sun. We find an intriguing parallel between the simulated spicular forest in a solar-like atmosphere and the numerous jets of polymeric fluid in the laboratory when both are subjected to harmonic forcing. In our radiative (both 2D and 3D) MHD simulations with sub-surface convection, the solar surface oscillations are excited similarly to those harmonic vibrations. A forest of spicules are formed in our simulations with heights ranging between 6 and 25 Mm, bearing substantially closer resemblance to clusters of jets observed in the solar atm