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.
Context. Analyzing extended emission in photometric observations of star-forming regions requires maps free from compact foreground, embedded, and background sources, which can interfere with various techniques used to characterize the interstellar medium. Within the framework of the NEMESIS project, we applied machine-learning techniques to improve our understanding of the star formation timescales, which involves the unbiased analysis of the extended emission in these regions. Aims.
Accurate quantification of regional ocean mass changes is crucial for coastal communities to formulate effective management strategies. The regional ocean mass budget comprises the barystatic component driven by terrestrial water and ice mass changes, and ocean mass redistribution resulting from non‐tidal oceanic and atmospheric (Nt‐OcnAtm), the latter being zero in the global mean.
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.
Context. Changes in the rotational period observed in various magnetized accreting sources are generally attributed to the interaction between the infalling plasma and the large-scale magnetic field of the accretor. A number of models have been proposed to link these changes to the mass accretion rate, based on different assumptions on the relevant physical processes and system parameters.
The neutral density perturbations exhibit multiscale features during geomagnetic storms, playing a crucial role in ionosphere‐thermosphere (I‐T) dynamics. However, the variations across various temporal and spatial scales remain underexplored. This study compared Gravity Recovery and Climate Experiment (GRACE) satellite data with simulations of Global Ionosphere‐Thermosphere Model (GITM) during the 2015 St. Patrick’s Day storm.
How do planetary systems, in general, and our own Solar System (SS), in particular, form? In conjunction, Astronomy and Isotope Cosmochemistry provide us with powerful tools to answer this age-old question. In this contribution, we review recent advances in our understanding of circumstellar disk evolution, including infall and disk processes, as explored through astrophysical models and nucleosynthetic isotope anomalies of SS materials.
Dust is studied on a range of scales, including large structures such as debris discs and smaller cometary tails. However, while astrophysical environments vary, dust particle dynamics is universal and crosses over into many research areas. A key influence on the dynamics of cosmic dust is radiation pressure, especially in the vicinity of stars. Here, we present an empirical relationship which accounts for radiation pressure forces deviating from the inverse square law.
From late October to early November 2003, one of the strongest recorded geomagnetic storms occurred due to heightened solar activity. Three ground‐level enhancement events (GLEs) took place during this period, GLE 65, 66, and 67, known as the Halloween events.
Plasma high-speed jets are common in Earth’s magnetosheath, and they significantly perturb the magnetosheath and affect the magnetosphere. The space environment of Mercury, characterized by the bow shock, magnetosheath, and magnetosphere, shares many similarities with that of Earth, so high-speed jets may also be formed in Mercury’s magnetosheath. Here we examine the formation of magnetosheath jets using a three-dimensional global hybrid simulation.
We present the PANORAMIC survey, a pure parallel extragalactic imaging program with JWST/NIRCam observed during Cycle 1. The survey obtained ∼530 square arcmin of NIRCam imaging from 1–5 μm, totaling ∼192 hr of science integration time. This represents the largest on-sky time investment of any Cycle 1 GO extragalactic NIRCam imaging program by nearly a factor of 2.
