{"total":11,"items":[{"citing_arxiv_id":"2606.25515","ref_index":58,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Accreting Compact Object Binaries with the SKA","primary_cat":"astro-ph.HE","submitted_at":"2026-06-24T07:48:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"This perspective paper outlines expected advances in studying accretion and jets in compact object binaries using the SKA's improved sensitivity and resolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12518","ref_index":28,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Black Hole Polarimetry III: Universal Polarization of Synchrotron Radiation at the Horizon","primary_cat":"astro-ph.HE","submitted_at":"2026-06-10T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Synchrotron polarization at the black hole horizon follows a universal pattern set solely by spin and inclination.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11322","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Ring Position Angles and Spin in M87* and Sgr A*","primary_cat":"astro-ph.HE","submitted_at":"2026-06-09T18:04:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GRMHD models show PA1 aligns with the approaching limb for high spins, enabling mild disfavoring of low spins and strong disfavoring of Earth-pointing spins in M87* from EHT data, with similar potential for Sgr A*.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.09326","ref_index":27,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Characterizing the Scale Height and Filamentary Structure of Radiatively Cooled MADs","primary_cat":"astro-ph.HE","submitted_at":"2026-05-10T04:59:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Radiative cooling in MADs above a transition accretion rate creates thinner denser filaments with increased efficiency, rendering conventional scale height measures misleading and motivating a new definition based on the polar position of the density maximum.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01002","ref_index":128,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Non-uniform particle injection into black hole jets by radiative magnetic reconnection","primary_cat":"astro-ph.HE","submitted_at":"2026-05-01T18:09:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Pair production via radiative magnetic reconnection near spinning black holes supplies non-uniform plasma to jets at levels sufficient to explain M87 radio emission.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.27332","ref_index":38,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Active Galactic Nucleus Feedback in an Elliptical Galaxy. IV. The Importance of the Jet Wind Coupling","primary_cat":"astro-ph.GA","submitted_at":"2026-04-30T02:20:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Jet and wind feedback from AGN couple nonlinearly through Kelvin-Helmholtz instability, raising energy dissipation efficiency to 0.64 and dropping star formation rate to 10^{-3} solar masses per year.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.23916","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GRRMHD Simulations of State Transitions in Non-Jetted Tidal Disruption Events","primary_cat":"astro-ph.HE","submitted_at":"2026-04-27T00:10:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GRRMHD simulations of TDE debris disks reveal thermal instability and collapse within weeks, producing soft X-ray excess followed by a sharp luminosity drop that resembles AT2021ehb observations.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"assume a distant observer whose camera sits at polar coor- dinates (θ, ϕ). Note that these coordinates are distinct from the fluid coordinates (r, ϑ, φ). Since the disk is symmetric and aligned with the BH spin, we simply useϕ= 0. Assum- ing blackbody emission, the frequency dependent luminosity from each cell is then dLr,ν(ν) =dL rfr(ϑ, φ, θ, ϕ) 15 π4νp \u0012 ν νp \u00133\u0010 eν/νp −1 \u0011−1 (29) for cell faces where bris the surface normal and dLϑ,ν(ν) =dL ϑfϑ(ϑ, φ, θ, ϕ) 15 π4νp \u0012 ν νp \u00133\u0010 eν/νp −1 \u0011−1 (30) for cell faces where± bϑis the surface normal. Hereν p = kTrad/h, andf r(ϑ, φ, θ, ϕ) andf ϑ(ϑ, φ, θ, ϕ) account for view- ing angle effects. The radial term is given by fr(ϑ, φ, θ, ϕ= 0) = cosϑcosθ+ sinϑsinθcosφ,(31) and the angular term is given by"},{"citing_arxiv_id":"2604.19435","ref_index":107,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"SDSSJ110546.07+145202.4: The first long-duration radio changing-look NLS1 galaxy","primary_cat":"astro-ph.HE","submitted_at":"2026-04-21T13:09:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SDSSJ110546.07+145202.4 is the first known long-duration radio changing-look NLS1 galaxy whose outburst is explained by an accretion-rate change that triggered a powerful radio jet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.06128","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"On the observational distinguishability of the Kerr and Kerr-Hayward metrics to EHT","primary_cat":"astro-ph.HE","submitted_at":"2026-04-07T17:40:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show the singularity-free Kerr-Hayward metric yields EHT observables that are functionally indistinguishable from the Kerr metric.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.02520","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Observational Properties of Near-Maximally Spinning Supermassive Black Holes","primary_cat":"astro-ph.HE","submitted_at":"2026-03-03T02:09:58+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GRMHD simulations at spins 0.9375 and 0.998 yield similar fluid properties and full-Stokes EHT images, indicating prior lower-spin runs remain representative for a ≳ 0.9375.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.09708","ref_index":58,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Development and Application of Numerical Techniques for General-Relativistic Magnetohydrodynamics Simulations of Black Hole Accretion","primary_cat":"astro-ph.HE","submitted_at":"2019-06-24T03:40:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Implements advanced GRMHD numerical techniques in Athena++ and demonstrates them via simulations of magnetically arrested disks around black holes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}