Listed are all scientific papers resulting from an ISSI activity written or co-authored by ISSI Team members, Working Group members, Workshop participants, visitors or staff members.
We present the new probabilistic model of the electron fluxes designed to assess the risks of the spacecraft surface charging for missions with near‐equatorial orbits in the inner magnetosphere. It is a second model developed within a frame of the European Space Agency’s activity “Plasma Environment Modeling in the Earth’s Magnetosphere” (PEMEM).
The polarity inversion line (PIL) in active regions (ARs) is considered to be closely associated with solar flare eruptions. In this study, we rigorously constructed standardized data sets based on time series of different lengths using Space‐weather HMI Active Region Patches (SHARP) parameters calculated along the PIL.
Cometary surfaces exhibit striking morphological diversity, with thick, smooth deposits abruptly transitioning to exposed bedrock and cliffs. This heterogeneity reflects spatially variable sublimation-driven erosion and sediment transport, yet how these processes combine to sculpt cometary surfaces remains poorly understood.
Accurate uncertainty information associated with essential climate variables (ECVs) is crucial for reliable climate modeling and understanding the spatiotemporal evolution of the Earth system. Recent developments in deep learning have remarkably advanced the estimation of ECVs with improved accuracy. However, the quantification of uncertainties associated with outputs of such deep learning models has yet to be widely adopted.
Mercury’s surface, as revealed by the MESSENGER probe, lacks distinctive absorption features in the visible–near-infrared spectral range, except for hollows that display a 630 nm feature ascribed to sulfides. The general absence of spectral features makes inference of its surface mineralogical composition challenging. We inspected the Praxiteles impact basin with newly photometrically corrected MDIS data, removing the influence of topographic shading in the spectra.
Bright points (BPs) are small-scale, dynamic features that are ubiquitous across the solar disc and are often associated with the underlying magnetic field. Using broadband photospheric images obtained with the Visible Broadband Imager at the National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST), the properties of BPs have been analyzed with DKIST for the first time at the highest spatial resolutions achievable.
Electrons of several hundred keV in Saturn’s ring current are important seed components of the radiation belt. In this study, we have statistically analyzed the spatial distribution of energetic electrons on the equatorial plane of the inner magnetosphere based on the Cassini in situ observations. We found for all energy channels, the peak position of energetic electron flux shifts from the midnight sector to the afternoon sector as L shell increases.
With recent observational advancements, exocomet studies have entered a new era: we have moved from an epoch where exocomets’ signatures were analysed to identify their true nature to a new epoch where individual exocomets’ detections are studied in detail to characterise the observed bodies. In this context, as with other astronomical objects such as exoplanets and minor bodies in the solar system, a nomenclature system is needed to uniquely identify any observed exocometary body.
Waves transport energy through the atmosphere without transporting mass. Often excited in the troposphere, they can propagate horizontally and vertically over long distances, depending on the type of wave and the background atmosphere. The fastest atmospheric waves are (infra)sound and acoustic gravity waves. The list of possible reasons for the generation of these atmospheric waves is not short; here, we concentrate on natural hazards.
When interplanetary magnetic field discontinuities interact with planetary bow shocks, hot flow anomalies (HFAs) form in the solar wind and can extend into the magnetosheath. Here we reconstruct the three‐dimensional geometry of an HFA bounded by two jet regions in the terrestrial magnetosheath.
