A new 3D non-LTE Ag I model atom yields a solar silver abundance of 1.15 ± 0.08, raising the prior value by 0.19 dex and shrinking the meteoritic offset to 0.06 dex.
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Time-series interferometry shows the Mira R Car pulsates steadily in the fundamental mode, while the red supergiant VX Sgr experiences episodic shock-driven mass loss and a pulsation-mode change.
3D NLTE sodium abundance corrections relative to 1D LTE are typically negative and larger for saturated lines in giants, reaching -0.7 dex, with a public grid released for use.
Planar very metal-poor stars exhibit chemical homogeneity and dwarf-galaxy-like abundance ratios, supporting origin from one ancient accreted system tentatively called Loki.
A revised parallel chemical evolution model with pre-enriched delayed second infall explains the Milky Way's alpha-element abundance patterns, co-evolution phase, and old low-alpha stars from APOGEE data.
PySME v1.0 introduces a revised line-selection framework and updated hydrogen-line physics to enable scalable, high-precision stellar spectrum modeling for large surveys.
NGC 6553 is a metal-rich globular cluster that formed in situ in the Galactic bulge, shown by its abundance patterns, multiple populations, and chemical DNA tests.
Monte Carlo tests with mock clusters show that fitting Gaia-like photometry with isochrones from different stellar codes produces biases of 0.6 to 1.5 in ΔY/ΔZ unless identical models are used for generation and fitting.
Asteroseismic ages from TESS calibrate [Y/Mg] and [C/N] chemical clocks, revealing a radially dependent [Y/Mg]-age relation that is steeper in the outer Galactic disc and flatter inward, with NLTE corrections and evolutionary stage accounting required for accuracy.
RV follow-up of 14 Gaia astrometric candidates identifies 6 binaries and confirms 8 substellar companions, updating binary contamination to 43%.
Planet-hosting wide binaries display diverse differential abundance trends with condensation temperature that are not universal across systems.
FLAME pipeline derives stellar luminosities, radii, masses and ages for Gaia DR4 using analytical calculations followed by minimization and Bayesian model inference, with tests showing statistical agreement to literature values.
Six seismic solar analogs have masses 0.91-1.04 solar masses, radii 0.95-1.08 solar radii, and ages 1.8-9.1 Gyr, with one star matching the Sun closely enough to be called a solar twin.
citing papers explorer
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Ag I model atom and the 3D non-LTE solar silver abundance
A new 3D non-LTE Ag I model atom yields a solar silver abundance of 1.15 ± 0.08, raising the prior value by 0.19 dex and shrinking the meteoritic offset to 0.06 dex.
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VLTI-GRAVITY measurements of cool evolved stars: II. Pulsation properties and mass-loss process of the Mira star R Car and the red supergiant VX Sgr
Time-series interferometry shows the Mira R Car pulsates steadily in the fundamental mode, while the red supergiant VX Sgr experiences episodic shock-driven mass loss and a pulsation-mode change.
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3D NLTE Sodium abundances in late-type stars. Abundance corrections and synthetic spectra
3D NLTE sodium abundance corrections relative to 1D LTE are typically negative and larger for saturated lines in giants, reaching -0.7 dex, with a public grid released for use.
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An ancient system hidden in the Galactic plane?
Planar very metal-poor stars exhibit chemical homogeneity and dwarf-galaxy-like abundance ratios, supporting origin from one ancient accreted system tentatively called Loki.
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Co-evolution of the Milky Way high- and low-{\alpha} sequences with chemical evolution models
A revised parallel chemical evolution model with pre-enriched delayed second infall explains the Milky Way's alpha-element abundance patterns, co-evolution phase, and old low-alpha stars from APOGEE data.
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PySME v1.0: improved modelling of stellar spectra for survey-scale applications
PySME v1.0 introduces a revised line-selection framework and updated hydrogen-line physics to enable scalable, high-precision stellar spectrum modeling for large surveys.
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The Bulge Cluster Origin (BulCO) survey with CRIRES at the ESO-VLT: a chemical screening of the Globular Cluster NGC 6553
NGC 6553 is a metal-rich globular cluster that formed in situ in the Galactic bulge, shown by its abundance patterns, multiple populations, and chemical DNA tests.
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A critical analysis of main-sequence fitting in open clusters to derive the helium-to-metal enrichment ratio $\Delta Y/\Delta Z$
Monte Carlo tests with mock clusters show that fitting Gaia-like photometry with isochrones from different stellar codes produces biases of 0.6 to 1.5 in ΔY/ΔZ unless identical models are used for generation and fitting.
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Calibration of the [C/N] and [Y/Mg] chemical clocks with asteroseismic ages from the TESS space mission
Asteroseismic ages from TESS calibrate [Y/Mg] and [C/N] chemical clocks, revealing a radially dependent [Y/Mg]-age relation that is steeper in the outer Galactic disc and flatter inward, with NLTE corrections and evolutionary stage accounting required for accuracy.
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The GAPS programme at TNG LXXV. Validating and confirming Gaia substellar astrometric candidates with HARPS-N
RV follow-up of 14 Gaia astrometric candidates identifies 6 binaries and confirms 8 substellar companions, updating binary contamination to 43%.
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Chemical signatures of planetary systems in their host stars. Near-infrared spectroscopy of four planet-hosting wide binaries
Planet-hosting wide binaries display diverse differential abundance trends with condensation temperature that are not universal across systems.
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Stellar masses and ages in Gaia Data Release 4 from the Final Luminosity Age Mass Estimator algorithm
FLAME pipeline derives stellar luminosities, radii, masses and ages for Gaia DR4 using analytical calculations followed by minimization and Bayesian model inference, with tests showing statistical agreement to literature values.
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Characterizing six seismic solar analogs observed by Kepler, K2, and HERMES
Six seismic solar analogs have masses 0.91-1.04 solar masses, radii 0.95-1.08 solar radii, and ages 1.8-9.1 Gyr, with one star matching the Sun closely enough to be called a solar twin.