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 emission of volatiles from the surface and subsurface of planetary bodies can provide fundamental knowledge concerning their formation, evolution, and structure. There are a variety of physical processes that shape the structural, kinematic and thermal behavior of the released material.
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.
Context. In the current panorama of large surveys, the vast amount of data that are obtained with different methods, data types, formats, and stellar samples prevents an efficient use of the available information. Aims. The Survey of Surveys is a project to critically compile survey results into a single catalog to facilitate the scientific use of the available information. In this second release, we present two new catalogs of stellar parameters (Teff, log g, and [Fe/H]). Methods.
Context. The young β Pictoris system has been monitored with high-resolution optical spectrographs for decades. These observations have revealed strongly variable stochastic absorption in the Ca II H&K lines attributed to infalling cometary bodies. Aims. Since 2003, over 9000 HARPS observations of β Pictoris have been taken, and many of these have not yet been used for exocomet studies.
Turbulence plays a crucial role in energy transfer from large to small scales in solar wind‐Venus interaction. Observations have identified magnetic field fluctuations and turbulence in the Venusian space environment. However, due to limited observations and simulation resolutions, neither the global characteristics nor the driving mechanisms of turbulence are settled.
