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.
Over five decades of space exploration have revealed that the Galilean moons—Io, Europa, Ganymede, and Callisto—exhibit a wide spectrum of geological and surface features shaped by the interplay of endogenous and exogenous processes. Each moon displays distinct characteristics: Callisto’s ancient, heavily cratered terrain; Ganymede’s contrasting dark and bright regions; Europa’s extensive fracture networks; and Io’s intense volcanic activity.
Plasma sheet electron precipitation into Earth’s atmosphere plays a key role in magnetosphere–ionosphere coupling at auroral latitudes. Such precipitation can be driven by four primary mechanisms that scatter equatorial electrons into the loss cone: resonant interactions with whistler‐mode waves, electron cyclotron harmonics (ECH), broadband electrostatic turbulence, and field‐line curvature scattering.
Magnetic switchbacks are large amplitude deflections of the magnetic field within the solar wind. They are Alfvénic in character and so are associated with a spike in velocity and a generally small variation in local plasma density. Early orbits of Parker Solar Probe revealed that the solar wind near the Sun is dominated by these structures, and therefore, they may be playing an important role in the energy budget and acceleration of the young solar wind.
Observations of continuous vertical electron and ion distributions at Jupiter were obtained simultaneously for the first time on 2023 September 7 UTC. On that date, Juno performed a radio occultation experiment and, in parallel, JWST and Keck scanned Jupiter’s limb, focused on characterizing H 3+ . Here, using Keck infrared spectra, we derive constraints on H 3+ densities and temperatures.
Shocks driven by coronal mass ejections (CMEs) are the most powerful accelerators of gradual solar energetic particles (SEPs) in the inner heliosphere. On 2023 March 13, a halo CME, as seen from the Solar and Heliospheric Observatory (SOHO) and the Sun TErrestrial Relations Observatory (STEREO), gave rise to a strong SEP event.
Turbulence is prevalent in astrophysical plasma flows. Both wave–wave interactions and coherent structures offer mechanisms to mediate turbulent cascades. Solar Orbiter in situ satellite observations of plasma turbulence in the solar wind are used to determine the percentage of the power in the turbulent cascade carried by coherent structures, and its anisotropy.
Collisionless shocks are fundamental accelerators of energetic particles, yet the observations of nonlinear foreshock structures, which are essential in acceleration processes, differ significantly between interplanetary (IP) shocks and planetary bow shocks.
The Voyager spacecraft (V1 and V2) provide unique in situ measurements of perturbations propagating beyond the heliopause through the very local interstellar medium (VLISM), including the shocks and pressure fronts whose origin is debated. In particular, a jump in magnetic-field strength, observed by V1 in 2020.4 at 149.3 au from the Sun, was followed by a distinct “hump” and persistently strong magnetic field, both requiring theoretical explanation.
Trends of essential climate variables are often estimated from climate data records to quantify changes in the Earth system. An understanding of the uncertainty in a trend is essential for accurately determining the significance of a trend and attributing its causes. Despite this importance, trend-uncertainty estimates rarely account for all known sources of uncertainty.
Context. A major challenge in modeling classical Cepheids is the treatment of convection, particularly its complex interplay with pulsation. This inherently three-dimensional (3D) process is typically approximated in one-dimensional (1D) hydrocodes, using dimensionless turbulent convection (TC) free parameters.
