{"total":11,"items":[{"citing_arxiv_id":"2606.23209","ref_index":60,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Parametrizing the projected wind fields of ultra-hot Jupiters in thermal emission: an application to GCM spectra of WASP-76b","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T11:53:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"dopplerkernel parametrizes UHJ projected winds with four parameters (v_jet, sigma_jet, v_wind, phi_sink) and retrieves jet and day-to-night flows from synthetic WASP-76b K-band emission spectra generated by three GCMs.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"an equatorial jet, and a source-sink flow. Let (x,y,z) be Cartesian coordinates in the observer frame, with ˆxpointing to the right, ˆy pointing upwards, and ˆzpointing toward the observer. Each point on the visible hemisphere lies on the unit sphere,x 2 +y 2 +z 2 =1 withz>0, so thatz= p 1−x 2 −y 2 is fully determined by the sky-plane coordinates (x,y). The orbital phaseϕ∈[0,1) is mea- sured from mid-transit (ϕ=0), and the corresponding rotation angle is 2πϕ. Solid-body rotation For a planet in synchronous rotation with equatorial velocityvrot, the zonal velocity at latitudeθisv rot cosθ. Sincex=cosθsinφ (whereφis the longitude), the LOS projection of the rotation velocity is v rot LOS(x,y)=v rot x.(A.1) Equatorial jet The equatorial jet is a zonal wind with a Gaussian latitudinal profile. Its LOS velocity is v jet LOS(x,y)=v jet xexp − y2 2σ2 jet  ,(A.2) wherev jet is the jet speed at zero latitude andσ jet is the standard deviation of the Gaussian, controlling how rapidly the jet speed decreases away from the equator. Thexfactor provides the same LOS projection as in Eq. (A.1). The rotation and jet terms share the same morphology but are physically distinct: rotation is a rigid-body term set by the planetary spin, while the jet represents a zonal wind anomaly superimposed on it. Source-to-sink flow The source-to-sink flow has a constant magnitudev wind every- where on the sphere. It diverges from a source at the substellar point and converges to a sink at longitudeφ sink on the equator, which is a free parameter of the fit. Whenφ sink =±180 ◦, the sink coincides with the antistellar point and the flow reduces to a classical day-to-night (i.e., substellar-to-antistellar) wind. The source and sink positions are defined in the co-rotating planet frame. However, we need to express them in the observer frame at a given phaseϕ. By definition, the planet frame co- incides with the observer frame atϕ=0 (mid-transit). With the source fixed at the su"},{"citing_arxiv_id":"2606.02083","ref_index":90,"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":"2605.20660","ref_index":33,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Formation of extremely low-mass white dwarf binaries undergoing enhanced angular momentum loss","primary_cat":"astro-ph.SR","submitted_at":"2026-05-20T03:26:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Enhanced angular momentum loss via outer Lagrangian point mass ejection in the Roche lobe overflow channel alters ELM WD structure and reproduces observed shorter orbital periods.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18950","ref_index":144,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Planetary formation tracks on the Hertzsprung-Russell diagram: Visualising the processes of giant planet growth","primary_cat":"astro-ph.EP","submitted_at":"2026-05-18T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Planetary formation tracks on the HR diagram show three branches: ascending during solid accretion with L proportional to T to the 8th for in-situ planetesimals, near-horizontal during gas accretion, and descending during post-accretion cooling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04141","ref_index":52,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Tale of a Hungry Subgiant and Its Brown Dwarf: Interior Radiative Damping Dominates the Tidal Evolution of TOI-5882","primary_cat":"astro-ph.SR","submitted_at":"2026-05-05T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A coupled MESA-GYRE framework shows interior radiative damping of gravity waves dominates tidal evolution in TOI-5882, predicting a 2-6 fold reduction in engulfment timescale versus equilibrium tide models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02766","ref_index":58,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.28135","ref_index":21,"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":"which may be written in terms of dimensionless gradient ∇as Frad = 4σT 4 3κρH ∇,(20) whereH=P/(ρg) is the pressure scale height and ∇ ≡dlnT /dlnP. The maximum radiative flux con- sistent with stability against convection is obtained by evaluating this expression at the largest temperature gradient permitted by the Ledoux criterion: ∇max =∇ ad + ϕ δ ∇µ.(21) In the radiative layer, we therefore have, ∇rad =∇ max = 3κP L 64πσGM T 4 ,(22) leading to a definition for the the maximum luminos- ity that can be transported without violating Ledoux stability: LLedoux = \u001264πσGM T 4 3κP \u0013 ∇max (23) evaluated at a representative location near the top of the Ledoux-stable region. The intrinsic luminosity is then"},{"citing_arxiv_id":"2604.18273","ref_index":182,"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":"2604.05049","ref_index":57,"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":22,"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},{"citing_arxiv_id":"2511.16859","ref_index":44,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Constructing Earth Formation History Using Deep Mantle Noble Gas Reservoirs","primary_cat":"astro-ph.EP","submitted_at":"2025-11-20T23:55:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}