{"total":17,"items":[{"citing_arxiv_id":"2606.31281","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The HST/WFC3 Transmission Spectrum of AU Mic b Part I: An Atmosphere Obscured by Contamination and Systematics","primary_cat":"astro-ph.EP","submitted_at":"2026-06-30T07:55:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The transmission spectrum of AU Mic b is dominated by the transit light source effect from stellar spots, yielding only weak atmospheric constraints with a preferred scale height below 185 km.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23774","ref_index":28,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"C, N, O, S, and photochemistry in a temperate giant planet orbiting a late M dwarf","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T18:00:00+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Transit spectrum of TOI-6894b indicates 3-10x solar metallicity with solar C/O, N/O, and S/O ratios, similar to Jupiter and Saturn.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06868","ref_index":141,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The mass of TOI-1883 b: A low density super-Neptune in the ridge regime transiting an early-M dwarf","primary_cat":"astro-ph.EP","submitted_at":"2026-06-05T03:35:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Mass of 13.7 Earth masses and density 0.4 g cm^{-3} measured for TOI-1883 b, a super-Neptune in the ridge regime around an early-M dwarf, with implications for disk migration and photoevaporation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06691","ref_index":34,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Ultraviolet Radiation Effects on the Optical Properties of Water-Dominated Exoplanet Hazes","primary_cat":"astro-ph.EP","submitted_at":"2026-06-04T20:13:33+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"UV irradiation makes water-dominated exoplanet haze analogs more absorbing from 0.5-8 μm, producing a detectable difference in the 2.6 μm N-H feature in modeled transmission spectra for GJ 1214b.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03824","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The CRIMSON survey I: super-stellar SiO in the directly imaged companion TWA 5 B from high-resolution M-band spectroscopy","primary_cat":"astro-ph.EP","submitted_at":"2026-06-02T16:07:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"High-resolution M-band spectroscopy detects super-stellar SiO in TWA 5 B, implying no significant magnesium-silicate clouds and formation consistent with core accretion beyond the CO snowline or gravitational instability with solid enrichment.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02083","ref_index":134,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Escape of Water- and Metal-enriched Atmospheres from compact Hot mini-Neptunes with CHAIN","primary_cat":"astro-ph.EP","submitted_at":"2026-06-01T11:14:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Water- and metal-rich atmospheres on compact hot mini-Neptunes lose mass more slowly than H/He cases at high enrichment levels due to enhanced cooling and higher mean molecular weight.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27353","ref_index":65,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Impact of Clouds on the Atmosphere-Mantle Interface of Sub-Neptunes","primary_cat":"astro-ph.EP","submitted_at":"2026-05-26T17:52:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Clouds drive over 1000 K heating at depth in sub-Neptune atmospheres, producing molten mantle interfaces for most planets in the sample and increasing abundances of O2, SiH4, and SiO by at least 36 percent.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15170","ref_index":42,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Role of Formation Location in Shaping Sulfur-, Nitrogen-, and Carbon-Bearing Species in Super-Earth and Sub-Neptune Atmospheres","primary_cat":"astro-ph.EP","submitted_at":"2026-05-14T17:55:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08752","ref_index":93,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Coupling magma-ocean and atmospheres in spectral retrievals of sub-Neptunes","primary_cat":"astro-ph.EP","submitted_at":"2026-05-09T07:27:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"MELTYQ couples magma-atmosphere equilibrium models with spectral retrievals to constrain sub-Neptune magma oxidation states and volatile inventories from transmission spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07833","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A New Global Chemical Equilibrium Code: Refractory Element Signatures in Super-Earths and Sub-Neptunes","primary_cat":"astro-ph.EP","submitted_at":"2026-05-08T15:03:07+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02036","ref_index":213,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"JWST unveils a high mean molecular weight atmosphere for mini-Neptune TOI-1130b: Evidence for formation beyond the water ice line","primary_cat":"astro-ph.EP","submitted_at":"2026-05-03T20:04:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.28135","ref_index":42,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Influences of Hydrogen-Silicate-Iron Miscibility on the Demographics of Sub-Neptunes and Super-Earths","primary_cat":"astro-ph.EP","submitted_at":"2026-04-30T17:18:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Models coupling hydrogen-silicate-iron miscibility with atmospheric escape reproduce the observed mass-radius occurrence density of sub-Neptunes and super-Earths.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"is parameterized by an initial saturated phase followed by power-law decay (e.g., Rogers & Owen 2021), LXUV(t) =    εXUVL⋆, t≤t sat, εXUVL⋆ \u0012 t tsat \u0013−α , t > t sat, (40) with the associated flux being FXUV(t) = LXUV(t) 4πa2 .(41) miscibility and sub-Neptune demographics11 The Roche geometric factor is taken to be (Salz, M. et al. 2016) K= 1− 3 2ξ + 1 2ξ3 ,(42) ξ≡ RL RXUV (43) with RL ≃a \u0012 Mp 3M⋆ \u00131/3 ,(44) whereM ⋆ is the stellar mass andais the planet's semi- major axis. The XUV absorption radius is parameterized as RXUV =R p +n H H(45) where the scale height is given by H= kBTtherm µ R2 p GMp .(46) HereR p is the photospheric radius,T therm is a char- acteristic upper-atmosphere temperature, andµis the"},{"citing_arxiv_id":"2604.24845","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"ORCHARD: A General Planetary Evolution Code","primary_cat":"astro-ph.EP","submitted_at":"2026-04-27T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"ORCHARD is a new open code that models planetary evolution and structure across terrestrial to gas giant masses using multiple equations of state and atmospheric boundary conditions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18301","ref_index":237,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Sensitivity of Dry Lava Planet Atmospheric Emission Spectra to Changes in Lava Compositions","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T14:06:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.07498","ref_index":39,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Hydrolyzed Hazes on Water-rich Exoplanets: Optical Constants and Detectability","primary_cat":"astro-ph.EP","submitted_at":"2026-04-08T18:35:50+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Hydrolyzed haze analogs from water-rich exoplanet conditions show higher absorptivity and a high imaginary refractive index that flattens spectral features in atmospheric models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.05049","ref_index":79,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Super-Solar Metallicity and Tentative Evidence for Photochemistry on WASP-96b from JWST and Ground-Based VLT Transmission Spectroscopy","primary_cat":"astro-ph.EP","submitted_at":"2026-04-06T18:01:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.21377","ref_index":39,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Coupled Thermal-Chemical Evolution Models of Sub-Neptunes Reveal Atmospheric Signatures of Their Formation Location","primary_cat":"astro-ph.EP","submitted_at":"2026-01-29T08:05:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}