A new histogram-free likelihood method applied to simulated JWST observations of brown dwarfs shows that globular cluster ages can be determined with formal errors under 0.2 Gyr.
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New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit
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abstract
We present new models for low-mass stars down to the hydrogen-burning limit that consistently couple atmosphere and interior structures, thereby superseding the widely used BCAH98 models. The new models include updated molecular linelists and solar abundances, as well as atmospheric convection parameters calibrated on 2D/3D radiative hydrodynamics simulations. Comparison of these models with observations in various colour-magnitude diagrams for various ages shows significant improvement over previous generations of models. The new models can solve flaws that are present in the previous ones, such as the prediction of optical colours that are too blue compared to M dwarf observations. They can also reproduce the four components of the young quadruple system LkCa 3 in a colour-magnitude diagram with one single isochrone, in contrast to any presently existing model. In this paper we also highlight the need for consistency when comparing models and observations, with the necessity of using evolutionary models and colours based on the same atmospheric structures.
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2026 48representative citing papers
Two young low-mass stars show solar C/O ratios while their inner disks are hydrocarbon-rich with C/O greater than one, providing direct evidence that disk processes enhance inner-disk carbon.
Radial velocity measurements of the brown dwarf CD-35 2722 B reveal a strong 169-day periodic signal attributed to a ~0.74 Jupiter-mass satellite, with a weaker secondary signal possibly indicating a second satellite near 2:1 resonance.
A new grid of disk models with grain-surface CO chemistry plus an ML inference tool produces gas mass estimates from ALMA observations that match independent dynamical and HD values without requiring extreme elemental depletion.
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HST/WFC3 UV imaging of SR 12 c measures accretion luminosity of 1.65 ± 0.19 × 10^{-5} L_⊙ and rate of 8 ± 2 × 10^{-12} M_⊙ yr^{-1}, placing it at the end stages of giant planet assembly with a full UV-to-sub-mm SED.
Ten new eclipsing WD + cool M-dwarf binaries found in TESS data via a targeted minute-scale eclipse search, increasing the TESS-discovered sample by an order of magnitude.
Planetary formation tracks on the HR diagram show three branches: ascending during solid accretion with L proportional to T to the 8th for in-situ planetesimals, near-horizontal during gas accretion, and descending during post-accretion cooling.
Joint speckle-atmosphere retrievals on JWST spectra of HD 19467 B and a field T dwarf detect H2O, CH4, CO, CO2 and NH3, yield carbon isotopic ratios of 154 and 85 respectively, and show near-solar metallicity with subsolar C/O.
An agnostic model using genetic algorithm optimization predicts photosynthetic viability declines linearly with orbital distance, expanding the photosynthetic habitable zone for M, K, and G stars beyond Earth-centric estimates.
Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.
Rest-frame optical galaxy SEDs from a 16-parameter SPS model are captured by five disentangled VAE latents (mass, young stars, dust, soft/hard ionization); metallicity and age are not independent drivers.
High-contrast imaging of HD 142527 reveals a candidate companion at ~14 au and an Hα spiral in the inner disk, possibly tracing accretion flows linked to companion B.
GJ 1132 b is estimated to have received at least 50 times the cumulative XUV flux of modern Earth with over 95% probability across models, supporting its classification as an atmosphere-free world.
FUor masses inferred from Keplerian line broadening in H-band spectra match the solar neighborhood IMF, indicating a universal eruptive phase during star formation.
N-body simulations find stellar mass-loss effects dominate gravitational scattering in altering giant planet orbits around white dwarfs formed in star clusters, independent of density and initial conditions.
Two extremely low-density Jupiter-sized planets on long-period orbits around TOI-791 were confirmed via ground-based photometry and TTV-derived masses.
Galaxy size-mass relations exhibit double power-law breaks at different pivot masses for quiescent versus bulge-dominated samples, coinciding with AGN activity scales.
Red dwarf mass-radius data from eclipsing binaries combined with dark-photon-inclusive evolution simulations produce competitive constraints on light dark photons.
An intercomparison of planetary evolution codes finds Earth magma oceans solidify in about 4 million years while Venus scenarios show more varied prolonged stages up to 50 million years, with outcomes sensitive to initial volatile budgets and model-specific treatments.
Generates and publicly releases 81,498 detrended Kepler light curves plus a catalog of 87 periodic variables (26 new) in the 2.5 Gyr cluster NGC 6819 using Gaia DR3 for membership.
Exo-REM k26 grids with f_sed and a two-column patchy-cloud framework fit VHS 1256 b with a 60-40 thick-thin split and reproduce the 10 μm silicate feature.
Simulations of the Aquila Rift show uneven clumps accreting gas and merging along filaments to form a fractal cluster whose velocity anisotropies, rotation, and expansion record the assembly history even after gas removal.
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.
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The Range of Cumulative XUV Flux on GJ 1132 b
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Inversion of Hydrogen-rich Atmosphere and Water Content for GJ 486b
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