JWST mid-IR observations of interstellar comet 3I/ATLAS yield the first direct methane detection and confirm strongly enhanced CO2:H2O mixing ratios relative to solar system comets.
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Phase-resolved high-resolution spectroscopy of CoRoT-2b measures sub-synchronous rotation at 2.6-sigma significance, consistent with its western hotspot offset.
A new redshift-correlation technique with third-generation GW detectors can constrain the BNS contribution to cosmic r-process nucleosynthesis to 5-6% precision via Fisher forecasts on mock bright- and dark-siren data.
The atmosphere of TOI-1130b shows high metallicity, low C/O, and elevated mean molecular weight consistent with ex-situ formation beyond the water ice line.
Hydrodynamical simulations of giant impacts find lower post-impact CMB pressures due to thermal and rotational effects, common full mantle melting, and conditions favoring metal-silicate equilibration near the CMB.
Deep Chandra data confirms three cold fronts in RXJ2014.8-2430 with widths indicating suppressed diffusion and identifies a concave structure consistent with either a Kelvin-Helmholtz instability or a powerful AGN cavity of radius 200-330 kpc.
Post-processing of 44-year adiabatic 3D simulations of common envelope events yields lightcurves with a 3-5 year hot peak from photosphere expansion, dust formation after 1-3 years causing bolometric decline and 400 K plateau, plus predictions of optical thinning in 100-200 years, matching some obse
Circulation models show equatorial jet strength most strongly alters Doppler shifts at ingress and egress, linearly affects mid-transit slope (secondary to rotation), and increases cross-correlation function width.
Detection of a micronova burst in TESS data of IGR J17014-4306, with inferred burned mass 1.6e-11 solar masses and recurrence time ~20 days, adding the eighth confirmed system.
Numerical model of C outgassing shows CC planetesimals deplete >50% carbon while NCs deplete <50% for typical sizes and formation times, favoring NC bodies as the main C source for terrestrial planets.
Accretion increases observable water mass in disks by expanding the emitting area via higher central luminosity, while viscous heating has no effect.
Using ray-tracing simulations and simulation-based inference, the authors construct an AGN population that reproduces the cosmic X-ray background, number counts, and absorption properties, deriving an intrinsic Compton-thick fraction of 40±3%.
Coupling Bern formation models with extended chemical equilibrium including S and N shows equilibration depletes atmospheric nitrogen, shifts C/O higher outside the ice line, generates Si species, and leaves sulfur abundances weakly dependent on formation location.
The -1 km/s absorption toward eta Tel is circumstellar with log C/O < -2.1, matching solar system comet abundances but not carbon-rich disks around hotter stars.
Sustained mass transfer from a circumbinary disc enables giant planet formation in gamma-Cephei-like binaries by prolonging the lifetime of the circumprimary disc against truncation and photoevaporation.
Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.
An optimal Stokes number window of 0.01-0.03 allows streaming instability to form planetesimals and pebble accretion to build all three main planet classes, with cold gas giants needing the lowest turbulence and largest discs.
Simulations indicate that order-of-magnitude changes in TiO2 and SiO2 abundances in lava melts produce distinguishable TiO, SiO, and SiO2 features in dry lava planet emission spectra, potentially observable with 12 JWST eclipses for the brightest targets.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
Revised solar photospheric abundances yield Z/X = 0.0187 with C, N, O at 8.46, 7.83, 8.69, preserving the solar modeling discrepancy and revealing a modest volatile-refractory offset from CI chondrites.
Observational study of 290 exoplanet-host stars finds higher C, O, S, Fe, Ni abundances in giant-planet hosts than small-planet hosts, with C/O ratios, hot/warm differences, and mass correlations that vary by subpopulation.
Barnard's Star planets have masses 0.19-0.84 M_earth, are tidally locked, unlikely to retain primary atmospheres, and possess mantles rich in ferropericlase with less than half Earth's water capacity and radiogenic heating.
New non-LTE abundances for three Bootes I stars show an alpha-element transition at [Fe/H] between -3 and -2, interpreted as the onset of type Ia supernova contributions in this ultra-faint dwarf galaxy.
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The chemical make-up of the Sun: A 2020 vision
Revised solar photospheric abundances yield Z/X = 0.0187 with C, N, O at 8.46, 7.83, 8.69, preserving the solar modeling discrepancy and revealing a modest volatile-refractory offset from CI chondrites.