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.
This article reviews the emerging field of exo-geoscience, focusing on the geological and geophysical processes thought to influence the evolution and (eu)habitability of rocky exoplanets. We examine the possible roles of planetary interiors, tectonic regimes, continental coverage, volatile cycling, magnetic fields, and atmospheric composition and evolution in shaping long-term climate stability and biospheric potential.
We present further results from the MUSE-ALMA Haloes survey, which includes 79 galaxies associated with strong H I absorption at z ∼ 0.5. As part of this effort, our ALMA Cycle 10 Large Program contributed new observations of 39 systems. This expands on the initial set of 21 systems in the MUSE-ALMA Haloes survey, bringing the total to 60 galaxies.
Prediction efficiency (PE) is a skill score that compares the data‐model metric of mean square error against the variance of the observations (i.e., using the average of the observed values as the “reference model” in the general skill score formula).
The search for life on exoplanets is difficult due to observational limitations stemming from vast separating distances. The Habitable Zone (HZ) is a simplifying framework for identifying exoplanets that may be suitable for life, given our observational limitations. The HZ framework is built on many simplifying assumptions and only attempts to bound the circumstellar regions where surface oceans are not precluded.
Climate-related sea level changes near the coast may deviate from what we observe in the open ocean. In effect, coastal changes result from the superposition of the global mean sea level rise, regional sea level trends, plus local contributions related to processes specific to nearshore areas. The latter operate on a broad range of timescales, from subdaily to multidecadal.
Several studies of Galactic cosmic-ray (GCR) modulation within the astrospheres of stars deemed to be proxies for the young Sun have concluded that the intensities of these particles would, at early stages of the Sun’s evolution, be negligible at 1 au. These studies, however, do not take into account the varying interstellar conditions the young Sun would have encountered as it traversed its Galactic orbit, nor do they realistically model the transport of GCRs.
Context. The direct empirical determination of the local value of the Hubble constant (H0) has markedly advanced thanks to improved instrumentation, measurement techniques, and distance estimators. However, combining determinations from different estimators is nontrivial due to their correlated calibrations and different analysis methodologies. Aims.
Energy transfer, cross‐scale coupling, and dissipation in astrophysical plasmas remain fundamental unresolved problems. The velocity‐shear–driven Kelvin–Helmholtz instability (KHI), ubiquitous in plasmas, is a key multiscale mechanism enabling plasma mixing, particle energization and the solar wind–magnetosphere coupling, making it a critical process for understanding how plasma flow energy is converted from large to kinetic scales.
This article reviews the short-, medium-, and long-term prospects for characterizing rocky exoplanets, a central goal of contemporary astrophysics. The primary objectives are to determine whether these planets host atmospheres; if so, to constrain their molecular composition and search for potential biosignatures; if not, to infer their surface composition and thereby enabling a form of exo-geology.
