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.
The solar wind (SW) bombards the surfaces of airless bodies like the Moon and Mercury, inducing sputtering that erodes regolith and sustains exospheres. While the sputtering yield has been given significant attention, the angular distribution of sputtered atoms remains underexplored for SW-like impacts, with prior studies confined to incidence plane measurements.
Solar analogs–stars that closely match the fundamental properties of the Sun–provide key benchmarks for testing stellar structure and evolution across different ages and activity levels. Their detailed characterization helps place the Sun into context within the broader population of solar-like stars. This study presents the characterization of six seismic solar analogs observed by the NASA Kepler and K2 missions.
During Type III solar radio bursts, beam-driven Langmuir/ -mode (upper-hybrid) wave turbulence is converted into electromagnetic emissions at the fundamental plasma frequency and its harmonics, through a chain of various linear and nonlinear wave processes.
Solar activity exhibits a range of quasi-periodic variations among different indices, reflecting the complex dynamics of the Sun. In this study, we investigate the temporal variation and hemispheric asymmetry of sunspot counts (SSC), sunspot areas (SSA), and X-ray solar flares during Solar Cycles 23 (SC23), SC24, and the ascending and maximum phase of SC 25 (1996–2024).
As an organic-rich world with a subsurface ocean, Titan is an object of great astrobiological interest. However, geological signs of surface-subsurface exchange are limited, and Titan’s thick icy crust may significantly impede delivery of organic-rich surface materials to the subsurface ocean.
Techniques developed in the past few years enable the derivation of multiscale ion convection and particle precipitation patterns from high‐resolution ground‐based observations, and it has been shown in previous studies that such multiscale geomagnetic forcing can contribute significantly to ionospheric and thermospheric disturbances. In this work, the global ionosphere–thermosphere model (GITM) is utilized to simulate the 27 March 2014 substorm event.
In the cometary plasma environment, the solar wind interacts with the expanding coma of heavy cometary ions. At high gas production rates, it can have plasma environment characteristics similar to the environment of Mars, with a bow shock and a cometosheath. Magnetosheath jets are transient enhancements in the dynamic pressure of the magnetosheath plasma. They can be generated at a disturbed bow shock surface and have been confirmed at Mars, Earth, and possibly Jupiter and Mercury.
We present quantitative investigations of the energy conversion pathways—electromagnetic ϵEM $left({{epsilon}}^{EM}right)$, fluid flow ϵf $left({{epsilon}}^{f}right)$, and particle thermal ϵth $left({{epsilon}}^{th}right)$ energies—within the Kelvin‐Helmholtz instability (KHI) observed by the Magnetospheric Multiscale mission.
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.
