Conveners
Poster Session 4.3
- Stefaan Poedts (KU Leuven)
Localized brightenings observed in extreme-ultraviolet (EUV) images, are generally interpreted as signatures of micro-or nanoflares occurring in the transition region or lower corona. These brightenings are omnipresent and hence, could well play a major role in heating up the solar corona. Recent observations with the Extreme Ultraviolet Imager (EUI) on board Solar Orbiter have revealed such...
Small scale solar vortices are ubiquitous in the photosphere, and they are believed to organize the magnetic fluxes, creating efficient conduits for energy transport and wave propagation. Another process linked to vortical flows is the generation of twisted magnetic flux tubes. In this work, the twisted magnetic flux is defined as a new typology of a solar vortex, and we applied forefront...
Five years ago, regular observations of the Sun with the Atacama Large Millimeter/sub-millimeter Array (ALMA) started. Since then, an increasing number of data sets have been acquired. At the same time, the Solar ALMA Pipeline (SoAP) for processing these data sets has been improved substantially. As a result, the first version of the Solar ALMA Science Archive (SALSA) was...
SDO/AIA images the full solar disk in several EUV bands that are each sensitive to coronal plasma emissions of one or more specific temperatures. We observe that when isolated active regions (ARs) are on the disk, full-disk images in some of the coronal EUV channels show the outskirts of the AR as a dark moat surrounding the AR. We will present several specific examples, selected from time...
The plasma in the solar corona originates from the photosphere and would, therefore, be expected to have similar elemental composition. However, elements with a low first ionisation potential (FIP) have been observed to have an increased abundance in certain regions of the corona. This phenomenon is known as the FIP effect and the degree of enhancement is measured using the FIP bias...
Since the discovery of the hot solar corona, a wide variety of mechanisms have been proposed for maintaining the high temperatures. The majority of these models fall into one of two broad categories, either AC (alternating current) or DC (direct current) heating. The distinction between these two groups arises from the characteristic time scales of the photospheric motions which are the source...
Both numerical simulations and observations of the solar atmosphere are limited in how small spatial variations they can resolve. The smallest processes in simulations are limited by the numerical grid employed, but the sun is under no such constraints. Therefore, observations and simulations at the same nominal resolution are not directly comparable, since sub-resolution effects not present...
