{"total":13,"items":[{"citing_arxiv_id":"2606.29895","ref_index":128,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Pristine composition or size evolution: Can current dust models reproduce emissivities observed in nearby protostars?","primary_cat":"astro-ph.GA","submitted_at":"2026-06-29T07:33:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28171","ref_index":74,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Demographics of planet-forming disks with the SKAO","primary_cat":"astro-ph.EP","submitted_at":"2026-06-26T15:03:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"SKAO will enable the first large-scale high-resolution surveys of cm-wavelength disk emission to constrain dust growth, pebble demographics, and planet formation processes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23801","ref_index":75,"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":"2606.23789","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2606.12862","ref_index":66,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Ultraviolet Imaging of SR 12 c with HST/WFC3: Accretion and Variability of a Giant Planet at the End Stages of Growth","primary_cat":"astro-ph.EP","submitted_at":"2026-06-11T03:46:28+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"HST/WFC3 UV imaging of SR 12 c measures accretion luminosity of 1.65 ± 0.19 × 10^{-5} L_⊙ and rate of 8 ± 2 × 10^{-12} M_⊙ yr^{-1}, placing it at the end stages of giant planet assembly with a full UV-to-sub-mm SED.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10624","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multi-epoch scattered-light analysis of HD 135344B: new evidence for a spiral-driving protoplanet","primary_cat":"astro-ph.EP","submitted_at":"2026-06-09T09:23:41+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-epoch analysis confirms 0.81 deg/yr spiral motion and co-moving twist in HD 135344B, consistent with a single protoplanet at 69 au driving multiple disk features.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.30023","ref_index":71,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An archival summary: 15 years of ALMA observations on disks and planet formation","primary_cat":"astro-ph.EP","submitted_at":"2026-05-28T14:42:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"ALMA observed 3933 independent coordinates in nearby star-forming regions for disks and planet formation, analyzed by sky location, frequency coverage, exposure time, spectral lines, and angular resolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05085","ref_index":211,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A formation pathway for giant planets in S-type discs of {\\gamma}-Cephei-like compact binaries","primary_cat":"astro-ph.EP","submitted_at":"2026-05-06T16:22:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Sustained mass transfer from a circumbinary disc enables giant planet formation in gamma-Cephei-like binaries by prolonging the lifetime of the circumprimary disc against truncation and photoevaporation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.21892","ref_index":144,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The impact of hydrogen atom tunneling on aromatic chemistry in TMC-1","primary_cat":"astro-ph.GA","submitted_at":"2026-04-23T17:44:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hydrogen tunneling makes H-abstraction reactions by C2H, OH, and CN competitive in TMC-1 despite low individual rates, affecting aromatic abundance predictions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19246","ref_index":53,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Ophiuchus DIsc Survey Employing ALMA (ODISEA). Substructures as a function of SED Class and disc mass in 100 systems","primary_cat":"astro-ph.EP","submitted_at":"2026-04-21T08:57:34+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"ALMA observations of 100 Ophiuchus discs show substructures linked to giant planet formation are common in discs above 10 Earth masses of dust and increase from Class I to Class II stages.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18332","ref_index":113,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dust characterization of halos: The extended emission in protoplanetary disks","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T14:31:54+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Halos in Elias 2-24, IM Lup, and DM Tau hold 20-30% of total dust mass with cm-sized grains, helping resolve the disk mass-budget problem even though drift and growth timescales are shorter than disk ages.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.17779","ref_index":21,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Exploring Polarized Millimeter Emission from Protoplanetary Disks with Irregular Dust Grains","primary_cat":"astro-ph.SR","submitted_at":"2026-04-20T04:03:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Irregular hexahedral dust grains yield nearly the same polarization morphology and fraction as spherical grains in self-scattering regimes but with up to 2.5 times higher scattering opacity, and are still insufficient to match observed polarization levels.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.09526","ref_index":50,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"High-Contrast Imaging of Forming Protoplanets: VLTs, JWST, and the Promise of ELT","primary_cat":"astro-ph.EP","submitted_at":"2026-04-10T17:46:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Reviews direct imaging of protoplanets and proposes deriving observational estimates of planet mass-to-radius ratio to test formation models, highlighting ELT capabilities.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"side of the ring, where the stellar light scatters on the rim. Interior of the cavity, the two confirmed accreting protoplanets PDS70 b and c are detected at high significance. The central star and an inner disk detected at radio wavelengths have been masked. left panel), and mass detection limits reach a sensitivity of∼2𝑀 𝐽 (Fig. 4, right panel) derived from the BEX isochrones [50]. A companion candidate has been identified at much larger separations (∼300 AU, see central panel of Fig. 4). Despite being consistent with the initial observations of spiral motion [94], more recent data spanning a longer baseline indicate that the spirals move together and the perturber responsible for launching them should be located around 66±3 au [95]."}],"limit":50,"offset":0}