{"total":10,"items":[{"citing_arxiv_id":"2607.08544","ref_index":143,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"How to measure tidal dissipation in long resonant chains","primary_cat":"astro-ph.EP","submitted_at":"2026-07-09T14:37:27+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A matrix-based extension of Papaloizou (2015) gives the tidal separation timescale T for N-planet chains and converts observed offsets into effective Q' bounds, with special sensitivity to the second and outermost planet masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30799","ref_index":126,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The GAPS programme at TNG: LXXVI. TOI-1533: a compact system hosting a super-Neptune-mass pair with disparate radii","primary_cat":"astro-ph.EP","submitted_at":"2026-06-29T18:22:15+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"TOI-1533 is confirmed as a rare compact system hosting an inner sub-Neptune and an outer hot super-Neptune-mass giant with nearly equal masses and very different radii.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23551","ref_index":128,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Observing a 542-day transiting giant with large TTVs: The 2025 transit of HIP 41378 f and new constraints on the outer system","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T16:25:34+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New 2025 transit timing for HIP 41378 f confirms large TTVs and is combined with prior data on planets d and e in an N-body model to update ephemerides and predict future transits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21625","ref_index":3,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The GAPS Programme at TNG LXXIV. A reanalysis of the planetary systems TOI-1272 and TOI-1694 with HARPS-N and retraction of the planetary interpretation of TOI-1272 c","primary_cat":"astro-ph.EP","submitted_at":"2026-06-19T17:29:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Reanalysis of TOI-1272 and TOI-1694 retracts TOI-1272 c as planetary, attributes the signal to stellar activity via Gaussian process modeling, and refines orbital parameters for the systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20803","ref_index":181,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Planet-Planet Secular Migration Predicts a Stellar Obliquity-Period Anti-Correlation","primary_cat":"astro-ph.EP","submitted_at":"2026-06-18T18:00:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Simulations show that von Zeipel-Lidov-Kozai migration from inclined companions produces misaligned short-period hot Jupiters while coplanar high-eccentricity migration preserves alignment at longer periods.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12010","ref_index":124,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.05295","ref_index":96,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"TOI-3664 b, TOI-4034 b & TOI-6564 b: Three new hot Jupiters around stars approaching the terminal age main sequence","primary_cat":"astro-ph.EP","submitted_at":"2026-06-03T18:00:07+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"TOI-3664 b, TOI-4034 b, and TOI-6564 b are three newly characterized hot Jupiters around terminal-age main-sequence stars, with sub-Jupiter masses and inflated radii.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"EEP values associated with Helium burning in the stellar atmosphere. Figure19.Atmosphericcharacterisationprospectsforthethreenewplanets. Alongside the planetary scale height and J-magnitude of their host stars, the TransmissionSpectroscopyMetric(TSM)foreachplanetisshownincolour, curtailedat200tobetterdifferentiatebetweentargetsneartherecommended follow-up (96) and first-quartile (159) cut-offs. TOI-6564b is particularly promising, with an atmospheric scale height of 645 km and TSM = 163. 𝐻𝑏 =𝑘𝑇 𝑒𝑞 /(𝜇𝑔 𝑏), where𝑘 𝑏 is the Boltzmann constant,𝜇is the mean molecular mass (assumed to be 2.3 amu here for a H/He at- mosphere), and𝑔 𝑏 is the planet surface gravity based in the derived mass and radius. Because of its host's brightness, TOI-6564b was"},{"citing_arxiv_id":"2606.04875","ref_index":122,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Model Selection Criterion for Multidimensional Gaussian Processes: Application to Radial Velocities","primary_cat":"astro-ph.IM","submitted_at":"2026-06-03T13:38:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Introduces MGIC_rv, an information criterion that combines conditional RV likelihood with an effective parameter count for selecting multi-GP models focused on radial velocities.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23469","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"TOI-7154b: A Close-in Massive Brown Dwarf in an Eccentric Orbit","primary_cat":"astro-ph.EP","submitted_at":"2026-05-22T10:27:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"TOI-7154b is a 71.7 M_J brown dwarf in an 8.86-day eccentric orbit around a G star, with eccentricity and age suggesting stellar-like fragmentation origins.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"αJ2000 17:38:16.88 (2) δJ2000 +15:12:48.73 (2) µα (mas yr−1) -11.072 ± 0.020 (2) µδ (mas yr−1) 9.558 ± 0.022 (2) ϖ† (mas) 3.346 ± 0.020 (2) d (pc) 292.901 ± 0.63 (2) Photometry: T 11.9445 ± 0.0066 (1) G 12.4247 ± 0.0003 (2) GBP 12.8087 ± 0.0007 (2) GRP 11.8792 ± 0.0005 (2) J 11.261 ± 0.021 (3) H 10.942 ± 0.027 (3) KS 10.858 ± 0.021 (3) W1 10.808 ± 0.023 (5) W2 10.855 ± 0.021 (5) W3 10.84 ± 0.118 (5) Spectroscopic parameters (TRES SPC): Teff (K) 5589 ± 50 (6) log g (cgs) 4.54 ± 0.10 (6) [Fe/H] (dex) 0 .14 ± 0.080 (6) v sin i∗ (km s −1) 3 .30 ± 0.50 (6) Derived stellar parameters: M∗ (M⊙) 0.939+0.047 −0.043 (6) R∗ (R⊙) 0.949+0.032 −0.030 (6) L∗ (L⊙) 0.782+0.036 −0.047 (6) ρ∗ (cgs) 1.55+0.18 −0.16 (6) Teff (K) 5564+100"},{"citing_arxiv_id":"2605.14433","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Where Do Hot Jupiters Come From? Revisiting Tidal Disruption and Ejection in High-Eccentricity Migration","primary_cat":"astro-ph.EP","submitted_at":"2026-05-14T06:27:25+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Planets with realistic dense cores survive close star encounters without total disruption, allowing more to circularize into hot Jupiters or be ejected after mass loss.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}