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.
An overview is presented of our current understanding and open questions related to magnetic reconnection in solar flares and the near-sun (within around 20Rs) solar wind. The solar-flare-related topics include the mechanisms that facilitate fast energy release and that control flare onset, electron energization, ion energization and abundance enhancement, electron and ion transport, and flare-driven heating.
It is well-known that the global acoustic oscillations of the Sun’s atmosphere can excite resonance modes within large-scale magnetic concentrations. These structures are conduits of energy between the different layers of the solar atmosphere, and understanding their dynamics can explain the processes behind coronal heating and solar wind acceleration. In this work, we studied the Doppler velocity spectrum of more than a thousand large-scale magnetic structures (i.e.
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.
Ionospheric molecular ions, such as N2+ ${mathrm{N}}_{2}^{+}$, NO+, and O2+ ${mathrm{O}}_{2}^{+}$, have been observed in Earth’s high‐altitude ionosphere and the magnetosphere by several spacecraft missions. Their presence not only indicates that they obtain sufficient energy through effective energization mechanisms, predominantly during the geomagnetically active times, but also provides clues regarding the connection between the ionosphere and the lower thermosphere.
We present a comprehensive analysis of 66 interplanetary shocks observed by the Parker Solar Probe between 2018 November and 2024 January. Among these, 33 events fulfilled the Rankine–Hugoniot (R-H) conditions, ensuring reliable asymptotic plasma parameter solutions. The remaining 33 events could not be confirmed by the standard R-H approach—potentially including wave-like structures—yet were analyzed via averaging and mixed-data methods to obtain robust shock parameters.
An International Space Science Institute (ISSI) workshop was convened to assess recent rapid advances in studies of magnetic reconnection made possible by the NASA Magnetospheric Multiscale (MMS) mission and to place them in context with concurrent advances in solar physics by the Parker Solar Probe, astrophysics, planetary science and laboratory plasma physics.
Classical Cepheids can be used as age indicators due to well-established period–age and period–age–color relations. G. De Somma et al. refined these relations by including a metallicity term and different mass–luminosity assumptions. In this study, we apply the period–age–metallicity relation for the first time to samples of classical Cepheids in M31 and M33. For both galaxies, we consider Cepheid coordinates and spatial distributions, along with the metallicity gradient by D.
Context. Alfvén wave solar models (AWSOMs) have been very successful in describing the solar atmosphere by incorporating the Alfvén wave driving as extra contributions in the global MHD equations. However, they lack the contributions from other wave modes. Aims. We aim to write governing equations for the energy evolution equation of kink waves. In a similar manner to AWSOM, we combine the kink-wave-evolution equation with MHD.
