{"total":13,"items":[{"citing_arxiv_id":"2606.31281","ref_index":29,"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":"2606.31017","ref_index":15,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Formation and evolution pathways of planets. I. Comparison between theory and observations","primary_cat":"astro-ph.EP","submitted_at":"2026-06-30T01:09:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Photoevaporative and collisional mass losses diversify exoplanet parameter space in ways consistent with standard core accretion, enabling an expanded eight-class classification scheme.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30644","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Testing the prevalence of hydrogen-silicate miscibility in young sub-Neptunes","primary_cat":"astro-ph.EP","submitted_at":"2026-06-29T17:59:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Hydrogen-silicate miscibility stores hydrogen in sub-Neptune interiors, resupplies escaping envelopes, delays contraction, matches young-planet observations, and enables a population test requiring 70-100 targets under 100 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18219","ref_index":23,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Ice Giants Revisited: Uranus and Neptune as Magma Ocean Worlds","primary_cat":"astro-ph.EP","submitted_at":"2026-06-16T17:48:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Uranus and Neptune are reinterpreted as magma-ocean giants with hydrogen-rich interiors rather than traditional ice giants, consistent with observations via three fit parameters each.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04283","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Preparing for the Early eVolution Explorer: Detecting the Primordial, Transiting Exoplanet Population","primary_cat":"astro-ph.EP","submitted_at":"2026-06-02T23:18:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A simulated 2.5-year multi-band photometric survey is projected to detect ~100 young transiting planets, sufficient to measure their occurrence rate to 5% precision and differentiate gas-dwarf versus water-world formation scenarios.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03740","ref_index":62,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"KRONOS I: The $1{-}2.8\\mu$m JWST Transmission Spectrum of the 23 Myr V1298 Tau c","primary_cat":"astro-ph.EP","submitted_at":"2026-06-02T14:55:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST NIRISS/SOSS data yield a transmission spectrum of the 23 Myr V1298 Tau c showing H2O absorption and an atmospheric metallicity of 14.8^{+56}_{-12} times solar, lower than mature planets of similar mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15170","ref_index":31,"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":"2605.07833","ref_index":22,"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":"2605.02766","ref_index":15,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Characterizing the bolometric-photoevaporative transition in young sub-Neptunes with radiation-hydrodynamic simulations","primary_cat":"astro-ph.EP","submitted_at":"2026-05-04T16:06:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"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.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"dient, which we take to be 2/7 for the H 2 dominated envelopes we consider here. This point is the radiative- convective boundary,R rcb. FromR rcb, we model the envelope as fully convective and adiabatic to the core radius,R c, which we approximate using a relation ap- propriate for an incompressible silicate of massM p (D. Valencia et al. 2006): Rc/R⊕ ≃(M p/M⊕)1/4.(15) This is also in practice the lowest the base of the atmo- sphere can be in our model. These atmospheric structures correspond to planet en- velope masses and energies that dictate the planetary evolution. The planet envelope mass can be found by integrating the density profile. The total available en- ergy for cooling is the sum of the available energy in"},{"citing_arxiv_id":"2604.28135","ref_index":28,"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":"method","top_context_polarity":"use_method","context_text":"binodal surface that separtes cores from overlying en- velopes. The non-ideal mixing between MgSiO 3 and H2 calculated by Gilmore & Stixrude (2026) is used here. Their density functional theory molecular dynam- ics (DFT-MD) simulations yield the binary free energy of mixing expression ∆ ˆGbinary mix = (LCBxH2 +L BC(1−x H2))x H2(1−x H2) × \u0012 1− T τ + P π \u0013 +RT(x H2 lnx H2 + (1−x H2) ln(1−x H2)), (28) whereL CB andL BC are the binary interaction parame- ters andx H2 is the mole fraction of H 2 along the binary join. The values for the subregular mixing parameters that fit DFT-MD simulations are:L CB = 622000 J/mol, LBC =−4950 J/mol,τ= 4800 K, andπ=−35 GPa. Gilmore & Stixrude (2026) find that addition of minor elements like Al has minimal effects on the position of"},{"citing_arxiv_id":"2604.20203","ref_index":18,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Sub-Neptunes Show a Stronger Correlation with Cold Jupiters than Super-Earths Especially in Metal-rich Systems","primary_cat":"astro-ph.EP","submitted_at":"2026-04-22T05:38:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Sub-Neptunes around metal-rich stars have a 42.6% conditional probability of cold Jupiters versus 14.5% for super-Earths, showing a metallicity-dependent correlation absent in the latter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18273","ref_index":201,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T13:48:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"An upgraded planet population synthesis model incorporates post-disc dynamical evolution and atmospheric enrichment to generate synthetic exoplanet populations with improved fidelity to N-body results and observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.21377","ref_index":25,"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}