{"total":32,"items":[{"citing_arxiv_id":"2606.26817","ref_index":53,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Investigating the System Configuration of Kepler-451 through Orbital Period Variations: Dynamical and Magnetic Interpretations","primary_cat":"astro-ph.SR","submitted_at":"2026-06-25T10:00:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Updated O-C diagrams for Kepler-451 favor a circumbinary planet at 3.4 AU after removing likely magnetic signals, with other LTT terms possibly systematic or magnetic in origin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25648","ref_index":51,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Long-term Orbital Period Variations of the Eclipsing Dwarf Nova HT Cas","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T09:57:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MCMC modeling of the O-C diagram for HT Cas indicates two circumbinary companions causing the long-term period variations, yielding a negative quadratic term consistent with standard CV evolution below the period gap.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25413","ref_index":64,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Resonant Super-Earths Dancing With EKL Oscillations: TTV Phase Excitation and Resonance Disruption by EKL Interactions between a Cold Jupiter and Stellar Companion","primary_cat":"astro-ph.EP","submitted_at":"2026-06-24T05:20:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations indicate EKL interactions excite TTV phases and disrupt resonances in a significant fraction of near-resonant super-Earth systems over 16 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23850","ref_index":34,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Dynamical implications of the recently detected feature around Quaoar and constraints on the presence of additional satellites","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T18:38:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical integrations favor interpreting the Quaoar occultation feature as a satellite rather than a triangular-point confined arc, while identifying stable regions for additional moons.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23789","ref_index":66,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Discovery of an Exterior Third Planet Orbiting $\\beta$ Pictoris","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Discovery of β Pic d, a 2-4 M_Jup planet at semi-major axis >30 au, via spectral template matching in JWST NIRSpec and MIRI data, confirmed by radial velocity and orbital stability.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23551","ref_index":292,"ref_count":1,"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":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New 2025 transit timing of HIP 41378 f shows a 7-hour early arrival consistent with TTVs; N-body modeling with TRADES refines ephemerides for planets d, e, and f.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23310","ref_index":190,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Barnard's Star Planetary System: Stability, Composition, and Evolution of Four Sub-Earth Exoplanets","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T13:24:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Barnard's Star planets have masses 0.19-0.84 M_earth, are tidally locked, unlikely to retain primary atmospheres, and possess mantles rich in ferropericlase with less than half Earth's water capacity and radiogenic heating.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23133","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Resonance and Stochastic Dynamics of Interplanetary Dust","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T10:24:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"UNKNOWN","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dust particles inspiraling under PR drag are temporarily trapped in MMRs, escape due to overstability of librations, then undergo stochastic scattering with predicted fractions for planetary collision, sublimation, or ejection via an analytic epicycle model and Monte Carlo method.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20224","ref_index":84,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.17348","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Clustering SPH Debris into N-body Fragments: A Collisional Code for Planet Formation","primary_cat":"astro-ph.EP","submitted_at":"2026-06-15T22:50:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SHARD is a collision-resolution framework that interpolates SPH results for remnants and clusters unresolved debris into N-body fragments while enforcing mass and water conservation for planet formation simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17344","ref_index":90,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"High-Eccentricity Tidal Migration Driven by Secular Chaos in Wide-Binary Systems","primary_cat":"astro-ph.EP","submitted_at":"2026-06-15T22:44:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Secular chaos regulated by the inner-to-outer ZLK timescale ratio R enables high-eccentricity tidal migration in 3+1 systems at sub-critical inclinations, producing polar hot Jupiters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02818","ref_index":55,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Nereid as a Regular Satellite of Neptune","primary_cat":"astro-ph.EP","submitted_at":"2026-06-01T19:35:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Nereid is proposed as Neptune's sole surviving regular satellite rather than a captured irregular satellite, based on new spectroscopic data and dynamical modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.01288","ref_index":28,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Is the Dark Comet 1998 KY$_{26}$ the Spacecraft Phobos 1?","primary_cat":"astro-ph.EP","submitted_at":"2026-05-31T15:19:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Orbital calculations indicate that 1998 KY26 could be Phobos 1 if the probe executed two burns totaling 1.9 km/s after its 1988 loss.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.30177","ref_index":62,"ref_count":2,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The Architecture of the 14 Herculis System Suggests Primordial Ejection of a Massive Planet","primary_cat":"astro-ph.EP","submitted_at":"2026-05-28T16:24:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N-body simulations show that 14 Herculis's orbital architecture requires primordial ejection of an additional massive planet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29150","ref_index":56,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Shock wave formation in the thermosphere by an earthgrazing fireball: Empirical evidence for volatile-enhanced hydrodynamic shielding","primary_cat":"astro-ph.EP","submitted_at":"2026-05-27T22:21:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Coordinated observations of a ~45 g earthgrazing fireball localize thermospheric shock generation to volatile-enhanced hydrodynamic shielding that enables continuum-like flow and detectable infrasound.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21579","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interstellar Medium-Driven Orbital Transport -- I. Radial Heating and Migration","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T18:00:01+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Realistic ISM fluctuations from TIGRESS-NCR MHD simulations drive stellar radial heating with σ_R ∝ t^{1/2} (early, cold) and t^{1/5} (late, warm) plus substantial migration explained by quasilinear theory with λ_* ~600 pc and τ_* ~70 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13409","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Comet 1P/Halley Completes 15 Orbits in 1,151 Years: Commensurability with the Solar System Quasi-Period and Evidence for Jupiter-Saturn Dynamical Coupling","primary_cat":"astro-ph.EP","submitted_at":"2026-05-13T12:04:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Comet Halley exhibits a precise 15:1 commensurability with a 1,151-year solar-system quasi-period, with Jupiter and Saturn providing coherent perturbation cancellation over that baseline.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12591","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Formation of stable exoplanetary systems around pulsars by capture: An exercise in computational classical mechanics","primary_cat":"astro-ph.GA","submitted_at":"2026-05-12T18:00:00+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N-body simulations demonstrate that post-capture chaotic planet-planet interactions around pulsars can produce stable low-eccentricity orbits after ejections.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12391","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Trajectory-Agnostic Asteroid Detection in TESS with Deep Learning","primary_cat":"astro-ph.EP","submitted_at":"2026-05-12T16:56:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A W-Net deep learning model detects asteroids in TESS data independently of trajectory by rotating training image cubes and using adaptive normalization for data scaling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"demonstrated using precision-recall (PR) curves or re- ceiver operating characteristic (ROC) curves. We will show both for clarity. Both PR curves and ROC curves evaluate the results at prediction thresholds, such that given labeled posi- tivesPand labeled negativesN, for prediction scoreq in the range [0,1], TP = X P:P i>q Pi (7) FP = X P:P i<q Pi (8) TN = X N:N i<q Ni (9) and FN = X N:N i>q Ni.(10) Precision and recall are defined as Precision = TP TP + FP (11) and Recall = TP TP + FN (12) It is important to emphasize that, with precision, we are mixing a quantity derived from the labeled positives (TP) with a quantity derived from the labeled nega- tives (FP), which will lead to lower precision values for brighter asteroids since there is a smaller quantity."},{"citing_arxiv_id":"2605.05293","ref_index":33,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Life is But a Stream: The Distribution of Planetary Systems Along Stellar Streams and their Properties","primary_cat":"astro-ph.EP","submitted_at":"2026-05-06T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show stars at the edges of stellar streams are more likely to retain unperturbed planetary systems than stars near the stream center.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01005","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Coordinate System for Dynamical Instabilities in Hierarchical Systems in REBOUND","primary_cat":"astro-ph.EP","submitted_at":"2026-05-01T18:19:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new wide-binary coordinate system in REBOUND's TRACE integrator produces qualitatively correct results for planet-planet scattering, stellar flybys, and ZLK oscillations where prior hybrid integrators fail, while matching IAS15 accuracy at up to 9x speed.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.26912","ref_index":94,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Eccentricity as a signature of hierarchical subsolar-mass mergers in collapsar disks","primary_cat":"astro-ph.HE","submitted_at":"2026-04-29T17:22:17+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25704","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Suppression of Resonant Overstability at Sharp Migration Gradients","primary_cat":"astro-ph.EP","submitted_at":"2026-04-28T14:30:38+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Sharp migration-rate gradients in protoplanetary disks quench resonant overstability when the dimensionless steepness parameter β exceeds the ratio of semi-major axis to eccentricity evolution timescales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24364","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Fates of the sub-stellar objects (FOSSO) II. Evidence for Suppression of Metal Pollution in White Dwarfs by Close Substellar Companions","primary_cat":"astro-ph.SR","submitted_at":"2026-04-27T11:59:19+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Close substellar companions suppress metal pollution in white dwarfs by a factor of 5.75 with 87% protection efficiency, backed by observations of 17 systems and N-body simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19743","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Viscously Stirring Particle Disks into Lorentzians and Gaussians to Infer Dynamical and Collisional Masses (ARKS XIII)","primary_cat":"astro-ph.EP","submitted_at":"2026-04-21T17:59:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Viscous stirring via gravitational scattering produces lognormal inclination distributions that yield Lorentzian vertical density profiles, which relax to Gaussians after equipartition, enabling estimates of perturber masses in ARKS debris disks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18252","ref_index":39,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Impact of Cold Jupiter Scattering on the Mean-Motion Resonance of Inner Small Planets","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T13:28:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Scattering cold Jupiters disrupt inner mean-motion resonances via secular perturbations from their orbital history, driving resonance circulation in most 2:1 and 3:2 configurations and explaining the Kepler period ratio distribution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.09184","ref_index":44,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Terrestrial planet formation in the era of GPU computing","primary_cat":"astro-ph.EP","submitted_at":"2026-04-10T10:12:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GPU-accelerated N-body simulations show that the common acceleration factor f distorts planetary chemical compositions and that terrestrial planets can form resonant chains without gas-driven orbital migration.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Terrestrial planet formation in the era of GPU computing 7 This hybrid symplectic integration method is implemented i n the Mercury code [10] and is very successful in simulating the formation of te rrestrial planets, and has been used in a large number of scientific publications ove r many years. Other commonly used codes are SyMBA [17], REBOUND [44], or GPLUM [2 8]. 2.4 Increasing /u1D475 The hybrid symplectic integrator described above and imple mented in the Mercury code [10] works very well for system sizes with /u1D441 < ≈ 2000. This limitation in the number of particles also limits the physical completeness o f the simulations. In this regime of /u1D441 , the initial body sizes are not much smaller than the Earth's moon."},{"citing_arxiv_id":"2604.08383","ref_index":70,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Planetesimal-Driven Instabilities in Resonant Chains of Cold Neptunes and Their Dynamical Outcomes","primary_cat":"astro-ph.EP","submitted_at":"2026-04-09T15:44:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Planetesimal disks with 1-4% of the planetary mass disrupt resonant Neptune chains, triggering instabilities that scatter planets to ~0.1 au orbits and enable hot Neptune formation on 10-100 Myr timescales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18597","ref_index":82,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Enhancement of the Rate of Tidal Disruption Events in Active Galactic Nuclei due to the Sweeping Secular Resonance Mechanism","primary_cat":"astro-ph.GA","submitted_at":"2026-04-02T04:06:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Sweeping secular resonance from an intermediate-mass companion and depleting disk enhances AGN TDE rates to 10^{-3}-10^{-2} per galaxy per year on Myr timescales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.11692","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Orbital Stability of Closely-Spaced Four-planet Systems","primary_cat":"astro-ph.EP","submitted_at":"2026-01-16T16:20:21+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Four-planet systems exhibit exponentially increasing lifetimes with orbital spacing, intermediate between three- and five-planet systems, with resonances causing shorter lifetimes and third-order MMRs adding destabilization near certain spacings.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.10666","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Observation Timelines for the Potential Lunar Impact of Asteroid 2024 YR4","primary_cat":"astro-ph.EP","submitted_at":"2026-01-15T18:33:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Asteroid 2024 YR4 has a 4.3% chance of striking the Moon in 2032, producing a 1 km crater with a visible optical flash, hours of infrared afterglow, magnitude-5 seismic reverberation, and escaping debris that could reach Earth.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.09835","ref_index":62,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"A Robust Launching Mechanism for Freely-Floating Planets from Host Stars with Close-in Planets","primary_cat":"astro-ph.EP","submitted_at":"2026-01-14T19:49:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Scattering between close-in super-Earths and secularly perturbed cold planets can launch some planets into free-floating orbits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}