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.
On 27 January 2017, Magnetospheric Multi‐Scale observed a series of electron vortexes, which are driven by the electron Kelvin‐Helmholtz (K‐H) instability in the reconnection outflow at terrestrial magnetopause. We find the electron vorticity can reach above 200 s−1 inside the vortexes, which is comparable to the strong vorticity events in the electron diffusion region.
Recent observations of the solar atmosphere in cool extreme-ultraviolet lines have reported the prevalence of coronal rain falling from coronal cloud filaments that are associated with the magnetic dips of coronal X-point structures. These filaments mysteriously appear as clouds of mass in the corona that subsequently shrink and disappear due to mass losses that drain as coronal rain along arced field lines.
Global temperatures in Jupiter’s upper atmosphere are poorly constrained. Other than an in situ measurement by the Galileo Probe, all temperature data come from remote-sensing methods that primarily rely on emissions from H 3+ , the dominant molecular ion in giant planet ionospheres.
We present a complete analysis of Fermi Large Area Telescope (LAT) data of GRB 221009A, the brightest gamma-ray burst (GRB) ever detected. The burst emission above 30 MeV detected by the LAT preceded, by 1 s, the low-energy (<10 MeV) pulse that triggered the Fermi Gamma-Ray Burst Monitor (GBM), as has been observed in other GRBs. The prompt phase of GRB 221009A lasted a few hundred seconds.
The evolution of magnetic braking and dynamo processes in subgiant stars is essential for understanding how these stars lose angular momentum. In this work, we investigate the magnetic braking and dynamo evolution of the G-type subgiant β Hyi to test the hypothesis of weakened magnetic braking and the potential rejuvenation of large-scale magnetic fields.
This review explores the anomalous transport and acceleration of charged energetic particles in heliospheric and astrophysical plasmas. Traditional diffusion-advection models can be insufficient to fully describe the observed behavior of energetic particles, prompting the need for alternative frameworks based on non-Gaussian stochastic processes and fractional differential equations to capture regimes of subdiffusion and superdiffusion of energetic particles.
The time-variable emission from the accretion flow of Sgr A*, the supermassive black hole at the Galactic center, has long been examined in the radio-to-millimeter, near-infrared (NIR), and X-ray regimes of the electromagnetic spectrum. However, until now, sensitivity and angular resolution have been insufficient in the crucial mid-infrared (MIR) regime. The MIRI instrument on JWST has changed that, and we report the first MIR detection of Sgr A*.
Tidal flats are the most important components of estuarine and coastal areas, playing vital roles in shoreline protection, ecological balance, and socioeconomic development. Various factors, including topography, tidal asymmetry, current-wave interactions, etc., have significant impacts on turbulence and sediment characteristics on tidal flats, thus controlling sediment transport and geomorphological evolution.
In the last 30 years, many papers reported the almost simultaneous occurrence of magnetospheric fluctuations at different frequencies and latitudes (basically, in the range f ≈ 1–5 mHz; T ≈ 200–1000 s) and the possible existence and stability of sets of favorite frequencies (in particular: f≈1 1.3, f≈2 1.9, f≈3 2.6–2.7, and f≈4 3.2–3.4 mHz) has been proposed, determining controversial results.
Coronal oscillations offer insight into energy transport and driving in the solar atmosphere. Knowing its polarization state helps constrain a wave’s displacement and velocity amplitude, improving estimates of wave energy flux and deposition rate. We demonstrate a method to combine imaging and spectral data to infer the polarization of a coronal loop’s standing kink wave, without the need for multiple instruments or multiple lines of sight.
