MELTYQ couples magma-atmosphere equilibrium models with spectral retrievals to constrain sub-Neptune magma oxidation states and volatile inventories from transmission spectra.
Title resolution pending
12 Pith papers cite this work. Polarity classification is still indexing.
12
Pith papers citing it
citation-role summary
background 2
method 1
citation-polarity summary
fields
astro-ph.EP 12representative citing papers
Young sub-Neptunes transition from core-powered bolometric escape to photoevaporative escape at smaller radii for lower-mass and more irradiated planets, with self-consistent simulations yielding combined mass-loss rates and analytic transition scalings.
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.
Hydrolyzed haze analogs from water-rich exoplanet conditions show higher absorptivity and a high imaginary refractive index that flattens spectral features in atmospheric models.
Coupled thermal-chemical models indicate that sub-Neptunes formed outside the water-ice line exhibit high atmospheric CH4, H2O, and C/O ratios while those formed inside show suppressed CH4 and low C/O.
An open-source GCE code with a 100x faster solver demonstrates that refractory ratios Mg/Si and Fe/Si control carbon partitioning and atmospheric properties in water-accreting sub-Neptunes.
Water-hydrogen demixing occurs on warm sub-Neptunes with envelope metallicities of 150-700 times solar, including TOI-270 d, implying layered interiors and underestimated bulk metallicities when using fully-miscible models.
High-resolution CRIRES+ spectroscopy yields a 3.6 S/N cross-correlation signal for CO2 in GJ 1214 b, with Bayesian retrievals giving metallicity 0.48, cloud deck pressure log Pc = -3.04, and temperature 398 K, consistent with JWST within 1.5 sigma.
WASP-96b shows super-solar metallicity of 2-6x stellar, roughly stellar C/O, tentative SO2 consistent with photochemistry, and an optical slope from scattering aerosols, supporting core-accretion formation beyond the water snowline.
Variable hydrogen-silicate-iron miscibility coupled with atmospheric escape reproduces the occurrence density structure, radius gap, and radius-period relation of sub-Neptunes and super-Earths based on accreted hydrogen fraction.
The Bern Model has incorporated MHD disk evolution, pebble accretion, and improved interiors, yielding quantitative matches to exoplanet mass functions, radius distributions, and system architectures.
citing papers explorer
-
The Influences of Hydrogen-Silicate-Iron Miscibility on the Demographics of Sub-Neptunes and Super-Earths
Variable hydrogen-silicate-iron miscibility coupled with atmospheric escape reproduces the occurrence density structure, radius gap, and radius-period relation of sub-Neptunes and super-Earths based on accreted hydrogen fraction.