{"total":11,"items":[{"citing_arxiv_id":"2606.27193","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stellar black hole binaries from two common envelope evolution phases in triple stellar systems","primary_cat":"astro-ph.HE","submitted_at":"2026-06-25T15:52:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A triple-star channel with two common envelope evolution phases produces merging black hole binaries with positive average χ_eff and a tail of negative values.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"0 infersκ z = 2.5±0.7 for the BBH population, consistent with the redshift evolution of the star-formation rate (Madau & Dickinson 2014). Withκ z = 2.5 the conversion factor is (1.2) −2.5 ≃0.633 and equation A3 maps the reported interval 27.5−49.4 Gpc −3 yr−1 to RBBH(z= 0)≃17.4−31.3 Gpc −3 yr−1.(A4) The uncertainty onκ z propagates only weakly: overκ z ∈[1.8,3.2] the factor ranges from (1.2) −1.8 ≃0.72 to (1.2) −3.2 ≃ 0.55, a∼15% spread that is subdominant to the width of the rate interval itself. As an independent check, the converted value is consistent with thez= 0 BBH rate reported directly by the earlier GWTC-4.0 analysis,R BBH = 14−26 Gpc −3 yr−1 (The LIGO Scientific Collaboration et al. 2025)."},{"citing_arxiv_id":"2606.23788","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Red vs. Blue: How metallicity shapes black hole dynamics and mergers in dense star clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"High-metallicity star cluster simulations produce black hole mergers with masses and ratios consistent with recent LVK detections, unlike low-metallicity models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11927","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Building three-dimensional giant stellar models for common envelope simulations","primary_cat":"astro-ph.SR","submitted_at":"2026-06-10T10:58:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Depositing stellar luminosity in an inner shell and cooling low-density outer cells produces a stable pulsating 3D red supergiant model for common envelope simulations without relaxation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29363","ref_index":15,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Sub-luminous Type IIP SN 2024abfl as a result of a significantly low energy Fe-core collapse","primary_cat":"astro-ph.HE","submitted_at":"2026-05-28T05:03:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SN 2024abfl is a sub-luminous Type IIP event from a compact progenitor exploding with energy at most 0.05 foe and nickel mass 0.003 solar masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28944","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Impact of the equation of state on core collapse supernovae I: the low-$T/|W|$ instability","primary_cat":"astro-ph.HE","submitted_at":"2026-05-27T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22938","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The first 3D MHD core-collapse progenitors II: Rotation, magnetic-field amplification, and magnetic topology","primary_cat":"astro-ph.SR","submitted_at":"2026-05-21T18:14:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"3D MHD simulations of pre-supernova Wolf-Rayet progenitors reveal cylindrical rotation and amplified small-scale magnetic fields that connect regions isolated in 1D models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22927","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The first 3D MHD core-collapse progenitors I: General properties, convection and nuclear burning","primary_cat":"astro-ph.SR","submitted_at":"2026-05-21T18:03:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"3D MHD simulations of pre-supernova progenitors find turbulent mixing in oxygen and silicon shells deviates from standard 1D mixing-length prescriptions, with proposed updates for stellar evolution codes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18951","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mapping 3-D Explosive Nucleosynthesis with Type II Supernova Infrared Emission Lines","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T18:00:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Late-time IR spectroscopy of SN 2024ggi shows varied line morphologies implying chemical inhomogeneity and aspherical ionization, with modeling favoring 12-15 solar mass progenitors but only high-mass energetic 3D simulations matching the observed Ni mixing extent.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12356","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Reproducing morphological features in the supernova remnant G11.2-0.3 by simulating jittering jets","primary_cat":"astro-ph.HE","submitted_at":"2026-05-12T16:30:41+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":"2605.10940","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Electromagnetic Follow-up of the Sub-Solar Mass Gravitational Wave Candidate S251112cm: Kilonova Constraints and a Coincident IIb Supernova","primary_cat":"astro-ph.HE","submitted_at":"2026-05-11T17:59:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"FAPcond =P \u0010 log10 I ≥log 10 ISN 2025adtq Hnull, N coincidence >0 \u0011 . (9) whereN coincidence is the number of simulated IIb SNe that fall within the three-dimensional localization region of S251112cm in a given trial. We find that FAPuncond = 1.926% and FAPcond = 43.932%. Now, assuming events of comparable significance are independent, P(C N) = [FAP]N .(10) Using this, we find that, in order to reject the null hypothesis with the unconditional probabilities, that we only need 2 (5) events like S251112cm and SN 2025adtq to achieve a 3σ(5σ) level of certainty. Given the con- ditional probabilities, we find that we will need 12 (26) events like S251112cm and SN 2025adtq to achieve a 3σ (5σ) level of certainty."},{"citing_arxiv_id":"2604.05019","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The neighboring stars of N6946-BH1 and the observational characteristics of failed supernovae","primary_cat":"astro-ph.SR","submitted_at":"2026-04-06T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N6946-BH1's remnant is roughly 10 times fainter than its progenitor while stellar merger remnants are 10-100 times brighter, and asymmetric dust cannot explain the difference.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}