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.
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.
The Cassini–Huygens mission (1997–2017) provided extensive data on the Saturnian system, which include observations of UV emissions from different objects in the system by the Cassini UV Imaging Spectrograph (UVIS). We present a modern, modular Python pipeline that delivers end-to-end processing of UVIS observations, from data reading and georeferencing to calibration.
The South Atlantic Anomaly (SAA) signicantly inuences particle dynamics and loss within the inner magnetosphere. Yet many inner magnetosphere models neglect the hemispheric magnetic‐eld asymmetry, leaving the impact of the SAA on ring current particles and the energy dependence of precipitation poorly constrained.
We present a multiline characterization of how oscillatory power is organized across distinct magnetic environments in an active region using seeing-free, stratospheric near-ultraviolet (near-UV) spectroscopy from the Sunrise iii UV Spectropolarimeter and Imager (SUSI). A 2 hr time series of short raster scans in the line-rich 327–329 nm window samples along a single transect that contains the following regions: weak magnetic field surroundings, a plage, a sunspot, and a pore.
Solar wind alpha particles exhibit preferential heating and acceleration relative to protons; however, their behavior in the vicinity of turbulent coherent structures remains less understood. We report the first evidence of localized alpha particle and proton heating within coherent structures identified using the Partial Variance of Increments (PVI) method based on Parker Solar Probe observations.
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.
Planetary upper atmospheres couple the deep atmosphere to the space environment. The dynamics and energetics of this rarefied, partially ionized region govern atmospheric evolution. At Jupiter, decades of past plasma measurements have revealed a variable and enigmatic ionosphere inconsistent with photochemical predictions and unusual global structures imprinted by the planet’s powerful magnetic field.
