{"total":63,"items":[{"citing_arxiv_id":"2606.29264","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Elemental Abundances from Off-center Carbon Burning in Accreting CO White Dwarfs: Implications for SN 2021yfj-like events","primary_cat":"astro-ph.SR","submitted_at":"2026-06-28T08:22:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical simulations find that off-center carbon burning in accreting CO white dwarfs produces substantial Si and S abundances that depend on initial carbon content, supporting the double WD merger scenario for SN 2021yfj-like events.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28506","ref_index":85,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Twin Peaks: Resolving Features in the Binary Black Hole Mass Function with 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dimming trend in rpTDE outbursts, supporting the Hills mechanism for orbit placement.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02700","ref_index":96,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Life and Death of Stars That Capture Primordial Black Holes","primary_cat":"astro-ph.HE","submitted_at":"2026-06-01T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Primordial black holes captured by stars lead to either quiet consumption or explosive disruption via disk formation, producing transients and high-spin remnants with potentially observable event rates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02539","ref_index":37,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"JWST's Little Red Dots as 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Milky Way, mostly in binaries, with metallicity and common-envelope ejection efficiency as the dominant shaping factors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14187","ref_index":239,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Distribution of Blue Straggler Stars in the Color-Magnitude Diagrams of Old Open Clusters","primary_cat":"astro-ph.SR","submitted_at":"2026-05-13T23:10:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Blue straggler stars in old open clusters predominantly appear near the terminal-age main sequence because mass transfer from asymptotic giant branch donors enriches their cores with 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Ergon et al. 2015), and were held fixed at their 2011dh-tuned values during the fit to 2025adtq. To infer explosion parameters for SN 2025adtq we ran a tiered parallel grid ofSuperSNECmodels vary- ing ejecta mass (controlled via the mass-excision coordi- nate, 1.5-2.1M ⊙), progenitor radiusR cut ∈[2,60]R ⊙, explosion energyE kin ∈[0.6,1.4]×10 51 erg, 56Ni mass 0.05-0.11M ⊙, two Ni mixing parameters, two ejecta 8 0 20 40 60 80 100 120 140 Days since best-fit t0 (MJD 60988.70) 17 16 15 14 13 12 11 AB absolute magnitude u g r i ²/N 1.0 range Figure 4.SuperSNEC-lcfit to theu/g/r/ilight curves of SN 2025adtq (Sec. 4.2.1). Filled circles: WFST + ZTF + ATLAS + PS1 + GOTO + Wendelstein photometry converted to absolute magnitude atd L = 140."},{"citing_arxiv_id":"2605.10610","ref_index":74,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"On the origin of variability in $\\alpha$ Cygni variable $\\epsilon$ Ori (HD 37128) using TESS observations and modelling","primary_cat":"astro-ph.SR","submitted_at":"2026-05-11T14:09:11+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Linear stability analysis and non-linear hydrodynamical simulations link the stochastic low-frequency variability of ε Ori to strange-mode instabilities that excite finite-amplitude pulsations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04591","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spectroscopic Disentangling Revealed the Tertiary Component in the Multiple System EM Boo","primary_cat":"astro-ph.SR","submitted_at":"2026-05-06T07:41:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Tertiary in EM Boo is A-F type with Teff=7000K; system distance ~300 pc indicates Gaia DR3 underestimates true distance due to multiplicity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04141","ref_index":85,"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":"2605.03500","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Interpreting Galaxy Physical Properties Using Stellar Population Synthesis","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T08:35:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The thesis assesses the reliability of stellar population synthesis modeling for galaxy physical properties using limited multi-band photometry rather than full spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03128","ref_index":88,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Double Neutron Star Delay Times Across Cosmic Metallicities: The Role of Helium Star Progenitors","primary_cat":"astro-ph.SR","submitted_at":"2026-05-04T20:10:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Population synthesis of helium star-NS systems yields DNS delay time distributions that peak between 80-250 Myr across metallicities, with 15% merging within 80 Myr and over 20% after 1 Gyr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01200","ref_index":104,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Type Ib Supernovae are bluer than Type Ic Supernovae","primary_cat":"astro-ph.HE","submitted_at":"2026-05-02T02:32:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Type Ib supernovae are systematically bluer than Type Ic supernovae in optical colors, likely due to helium-rich versus helium-poor progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24596","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Theoretical Study of the Structure and Elemental Abundances of HD 20794","primary_cat":"astro-ph.SR","submitted_at":"2026-04-27T15:20:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"MESA grid models find HD 20794 is a 0.80 solar-mass star aged ~9 Gyr whose observed abundances match core-collapse supernova enrichment and are preserved over Gyr timescales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20010","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The First Infrared Portrait of A Solar-Like Host Star with Debris Disk: Pioneering High-Resolution H- and K-Band Spectroscopy of HD115617 with Comparative Optical Spectrum Analysis","primary_cat":"astro-ph.SR","submitted_at":"2026-04-21T21:39:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The first NIR high-resolution spectroscopy of solar analog HD115617 shows a 250 K temperature discrepancy with optical data but confirms solar composition, main-sequence status, and no chemical signature of planetary formation.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"(2005), [11] Soubiran & Girard (2005), [12] Valenti & Fischer (2005), [13] Reddy et al. (2006), [14] Takeda et al. (2007), [15] Ram'ırez et al. (2007), [16] Sousa et al. (2008), [17] Holmberg et al. (2009), [18] Mena et al. (2010), [19] Ghezzi et al. (2010), [20] Gonzalez et al. (2010), [21] Prugniel et al. (2011), [22] Adibekyan et al. (2012), [23] Ram 'ırez et al. (2012), [24] Maldonado et al. (2012), [25] Da Silva et al. (2012), [26] Ram 'ırez et al. (2013), [27] Tsantaki et al. (2013), [28] Bensby et al. (2014), [29] Nissen et al. (2014), [30] Battistini & Bensby (2015), [31] Da Silva et al. (2015), [32] Sitnova et al. (2015), [33] Bonfanti et al. (2016), [34] Zhao et al. (2016), [35] Brewer et al. (2016), [36] Stassun et al."},{"citing_arxiv_id":"2604.18688","ref_index":58,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"White dwarf + M dwarf Detached Binaries in Long Period Radio Transients: Observed Binary Parameters, Evolution, and Population Constraints","primary_cat":"astro-ph.SR","submitted_at":"2026-04-20T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Two long period radio transients are detached white dwarf-M dwarf binaries with matching periods, massive cool crystallized white dwarfs, low inclinations, and an estimated population of 100-2000 such systems within 2 kpc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18579","ref_index":78,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The T16 Planet Hunt: 10,000 New Planet Candidates from TESS Cycle 1 and the 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g-dominated mixed modes in four red giants suggest convective overshooting rises with mass and yield a core rotation rate of 0.7409 μHz for KIC 11968334.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.13604","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Irregularly Sampled Time Series Interpolation for Binary Evolution Simulations Using Dynamic Time Warping","primary_cat":"astro-ph.SR","submitted_at":"2026-04-15T08:13:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dynamic Time Warping with a shared warping path across parameters aligns binary stellar tracks for accurate interpolation while preserving physical relationships such as the Stefan-Boltzmann 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