{"total":22,"items":[{"citing_arxiv_id":"2606.30438","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"CARMApy: An Open-Source Python Framework for Simulating Microphysical Clouds in Planetary Atmospheres","primary_cat":"astro-ph.EP","submitted_at":"2026-06-29T15:13:37+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"CARMApy provides a Python interface to the ExoCARMA microphysics code, enabling simulation of cloud particle size distributions and rates in exoplanet atmospheres with claimed consistency to prior versions and speed gains of 1.9x single-threaded and 3.8x multithreaded.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"they are small and slow moving) and thus their sedimentation velocity,v t, can be described by Stokes' fall velocity vt = 2 9 gr2Cc (ρp −ρ a) ηa −v winds (30) wheregis the gravitational acceleration,v winds is a user defined upward wind speed, andC c is the Cunningham slip factor which is given by (N. A. Fuchs 1964, Eqn. 8.5) Cc = 1 + Kn \u0010 1.256 + 0.42e−0.87/Kn \u0011 (31) where the numerical constants in this equation are empirically derived from falling oil drops and Kn is a Knudsen number given by: Kn = ℓ r = 2ηa ρa r πMa 8RT (32) The Reynolds number is defined as follows Re= 2rρa(vt +v winds) ηa (33) IfRe <1 then our assumption that particles are small and slow moving is valid and we use Equations 30 and 33 for"},{"citing_arxiv_id":"2606.29552","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Improving the Precision of Line-by-Line Radial Velocities: A Data-Driven Iterative Algorithm for Spectral Line Selection","primary_cat":"astro-ph.EP","submitted_at":"2026-06-28T18:34:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FLARES iterative line-selection algorithm achieves 1.122 m/s RV RMS using 24 lines on 383 days of NEID solar data, better than full list or CCF.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27252","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Improving exoplanet mass characterisation with Bayesian model selection using the Learned Harmonic Mean Estimator","primary_cat":"astro-ph.EP","submitted_at":"2026-06-25T16:37:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First use of the learned harmonic mean estimator for Bayesian model selection across circular/eccentric, white-noise/GP, and trend variants in radial velocity exoplanet analyses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26343","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Architectures of Planetary Systems III: Excitation of Eccentricities and Inclinations","primary_cat":"astro-ph.EP","submitted_at":"2026-06-24T19:36:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Gapped planetary systems and those with detected outer planets show higher eccentricity excitation than compact systems, with a predicted population of highly inclined long-period planets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23801","ref_index":32,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Direct Imaging Discovery of Giant Exoplanet $\\beta$ Pictoris d: A Decade-Long Game of Hide-and-Seek","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Direct imaging discovery of β Pictoris d, a ~2.4 M_Jup planet at ~26 au with CO2-rich atmosphere, detected in multi-epoch VLT and JWST observations and consistent with bound orbital motion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20789","ref_index":14,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dynamical Tides during High-Eccentricity Migration produces the Hot Jupiter Pile-up, Neptune Ridge, and Neptune Desert","primary_cat":"astro-ph.EP","submitted_at":"2026-06-18T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Dynamical tides exciting f-modes during high-eccentricity migration produce the hot Jupiter pile-up, Neptune ridge, and Neptune desert via orbital circularization and selective atmospheric mass loss.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20224","ref_index":300,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"TOI-2147 b and TOI-6019 b: Two eccentric warm Jupiters detected and characterized with TESS and MaHPS","primary_cat":"astro-ph.EP","submitted_at":"2026-06-18T13:38:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Detection and characterization of two eccentric warm Jupiters TOI-2147 b (P=26.2 d, e=0.29, M=116 M⊕) and TOI-6019 b (P=14.5 d, e=0.48, M=149 M⊕) with TESS and MaHPS data, showing mildly inflated radii consistent with tidal heating.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12010","ref_index":222,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The 35-Myr old infant planet TOI-837 b has a mildly misaligned orbit","primary_cat":"astro-ph.EP","submitted_at":"2026-06-10T12:33:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"TOI-837 b has a true obliquity of 25.9+7.5-6.3 deg, the first planet younger than 100 Myr with accessible ψ incompatible with an aligned orbit, favoring primordial disc torque followed by disc-driven migration.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11330","ref_index":23,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Do Super-Puffs Defy Core Accretion? Population-Wide Interior Structure Constraints","primary_cat":"astro-ph.EP","submitted_at":"2026-06-09T18:10:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Interior structure models show 28 of 34 cold super-puffs are consistent with core accretion while six require non-standard explanations such as impacts or exo-rings.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09973","ref_index":191,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stellar Obliquities of Young Systems, Atmospheres Undergoing Contraction and Escape (SOYSAUCE) II: a 135 Myr planet on an aligned orbit with transit timing variations","primary_cat":"astro-ph.EP","submitted_at":"2026-06-08T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validation of a 135 Myr, 3.6 R_E transiting planet with aligned obliquity and TTV evidence for a near-resonant companion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06234","ref_index":104,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"gr8stars II : judgement day for spectroscopic parameter model systematics","primary_cat":"astro-ph.SR","submitted_at":"2026-06-04T14:39:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-method spectroscopic analysis of 585 FGK dwarfs shows parameter scatters larger than internal errors, inducing sub-5% fractional uncertainties on derived exoplanet radius and mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28719","ref_index":104,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Homogeneous Catalog of Rossiter-McLaughlin Systems: Distinct $e$-$\\lambda$ Trends in Three Gas-Giant Mass Regimes","primary_cat":"astro-ph.EP","submitted_at":"2026-05-27T16:39:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Homogeneous reanalysis of 145 single-star RM systems reveals mass-dependent e-λ trends: sub-Saturns eccentric and misaligned, Jupiters misaligned only when circular, and super-Jupiters aligned at all eccentricities.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23018","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Gaia Exoplanet Orbits, Demographics, and Evolution Survey (GEODES): Characteristics of Three Long-Period Companions Accelerating their Host Stars","primary_cat":"astro-ph.EP","submitted_at":"2026-05-21T20:41:14+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Three accelerating stars yield one stellar companion at 166 AU, one 45 Jupiter-mass object at ~18 AU, and one 9.5 Jupiter-mass object at 6.4 AU that is 65% likely to be a planet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18949","ref_index":31,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mars as an Exoplanet: Lessons from a Planet at the Edge of Habitability","primary_cat":"astro-ph.EP","submitted_at":"2026-05-18T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Mars provides a real-world case study of processes like volatile loss, climate evolution, and magnetism that determine habitability on small rocky planets at the edge of habitable conditions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11075","ref_index":23,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Uniform Determination of the Bulk Metallicities and Alpha Enrichments of Confirmed Exoplanet Systems with TRES","primary_cat":"astro-ph.EP","submitted_at":"2026-05-11T18:00:03+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A uniform spectroscopic catalog of 625 exoplanet hosts shows subsolar-metallicity giant-planet hosts are alpha-enhanced relative to both iron-rich hosts and typical metal-poor field stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07392","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mass Production of 2023 KMTNet Microlensing Planets. III: Three Planets from the Subprime Field","primary_cat":"astro-ph.EP","submitted_at":"2026-05-08T07:47:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Three new planets detected via 2023 KMTNet microlensing with mass ratios log q ~ -1.9, -2.0, -2.6; overall 2023 sample of 25 planets matches prior mass-ratio distribution.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2023 (AlertFinder) Figure 13.Cumulative distributions oflogqfor KMTNet Anoma- lyFinder planets from all 2016-2019 events (black curve) and from 2023 AlertFinder events (red curve), adapted from Figure 15 of Gui et al. (2024). The mass ratio of each planet is adopted from the best-fit model. The dark turquoise region indicates the \"sub-Saturn desert\" (logq= [−3.6,−3.0]) indicated by Zang et al. (2025). 1592 (logq=−3.010, Li et al. 2026), are located near its boundary. At present, among the 890 events newly identified by the end-of-year KMTNet EventFinder pipeline (Kim et al. 2018a), only two stellar binary events with prominent orbital effects (Han et al. 2024e) and one free-floating planetary event have been published (Jung et al."},{"citing_arxiv_id":"2604.18579","ref_index":21,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The T16 Planet Hunt: 10,000 New Planet Candidates from TESS Cycle 1 and the Confirmation of a Hot Jupiter Around TIC 183374187","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T17:59:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A transit search on TESS Cycle 1 full-frame images produced 10,091 new planet candidates down to T=16 mag, more than doubling the known TESS total, with one hot Jupiter confirmed by radial velocity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18281","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Two Potential Exoplanets around A-type Stars Selected from 18 Planetary Candidates","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T13:54:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Two TESS candidates around A-type stars are flagged as promising exoplanets after low false-positive probabilities are calculated for 18 screened objects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16297","ref_index":15,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"TTV-Not-So-Fast: Uniqueness and Degeneracy in Perturbing Planet Parameters","primary_cat":"astro-ph.EP","submitted_at":"2026-04-17T17:59:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Reassessment of 12 TTV claims finds only two systems with compelling unique solutions for the perturbing planet, six with multiple viable solutions, and two with weak evidence overall.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.07598","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"On the Information Content of Ariel Transmission Spectra: Reassessing the Tier System","primary_cat":"astro-ph.EP","submitted_at":"2026-04-08T21:08:18+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Tier 1 Ariel spectra suffice for sub-1.5 dex constraints on H2O and CO2 in giant-planet atmospheres, with higher tiers providing only incremental gains and more molecules in select cases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.05049","ref_index":30,"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":"2603.01534","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Intrinsic Multiplicity Distribution of Exoplanets Revealed from the Radial Velocity Method. II. Constraints on Giant Planet Multiplicity from Different Surveys","primary_cat":"astro-ph.EP","submitted_at":"2026-03-02T07:03:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Giant planet multiplicity is low, with 10.6% and 15.8% of Sun-like stars hosting at least one giant planet within 10 au across the two surveys, mostly as singles, inconsistent with scattering models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}