{"total":15,"items":[{"citing_arxiv_id":"2606.30886","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multipolar Magnetic-Field Inference for PSR J0740+6620 with Neural-Network-Accelerated NICER Pulse-Profile Modeling","primary_cat":"astro-ph.HE","submitted_at":"2026-06-29T20:22:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Neural-network surrogate accelerated MCMC infers multipolar magnetic field parameters for PSR J0740+6620 from NICER data, finding broad multimodal posteriors and disfavoring a zero-offset model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.29146","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Neutron Star Mass across Binary Pulsar Subpopulations: Mass-Spin Correlation, Mass Distributions, and Moment of Inertia Effects","primary_cat":"astro-ph.HE","submitted_at":"2026-06-28T01:55:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Hierarchical Bayesian analysis of ~50 binary pulsars finds moderate evidence for mass-spin anti-correlation (ρ = -0.26) in the recycled population, plus a small mass offset by white-dwarf companion type and confirmation of companion-mass–eccentricity correlation in DNS systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27852","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mass-Ratio Reversal as an Alternative to Hierarchical Mergers for GW241011","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T08:47:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Mass-ratio reversal in isolated binaries offers a viable formation path for GW241011-like events under specific stellar-evolution and interaction conditions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23926","ref_index":56,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854","primary_cat":"astro-ph.HE","submitted_at":"2026-06-22T20:44:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10964","ref_index":86,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The link between obscured accretion and mildly relativistic precessing jets","primary_cat":"astro-ph.HE","submitted_at":"2026-06-09T15:03:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Observational evidence links obscured super-Eddington accretion to slower precessing jets in stellar-mass compact object systems, contrasting with fixed fast jets in low-density environments.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05842","ref_index":90,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The X-ray emission of the long-period transient and accreting cataclysmic variable ASKAP J174508.9-505149","primary_cat":"astro-ph.HE","submitted_at":"2026-06-04T08:17:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"X-ray timing and spectral analysis of ASKAP J174508.9-505149 detects matching periodicity and features consistent with an accreting magnetic CV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21580","ref_index":260,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18731","ref_index":157,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T17:53:13+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15724","ref_index":4,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Pilot Study of Mildly Recycled Pulsars: A Case Study of PSR J2338+4818","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T08:21:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Follow-up observations of PSR J2338+4818 detect 27,228 single pulses with no nulling and measure scintillation timescales of 2.93-25.26 min and bandwidths of 1.68-27.41 MHz.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.09637","ref_index":21,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A NICER and AstroSat view of the neutron star low-mass X-ray binary 1A 1246-588","primary_cat":"astro-ph.HE","submitted_at":"2026-05-10T16:33:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-epoch observations of 1A 1246-588 show blackbody temperature rising from 0.28 to 0.39 keV with emitting radius 6.9-13.8 km and Comptonization photon index varying 1.8-2.3, consistent with atoll-state changes from accretion power redistribution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19534","ref_index":60,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The swept-back multipolar magnetic field of neutron stars: Application to NICER MSP J0030+0451","primary_cat":"astro-ph.HE","submitted_at":"2026-04-21T14:53:46+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A centered swept-back multipolar magnetic field up to octupole order reproduces the bolometric thermal X-ray light curve of MSP J0030+0451.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.05406","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Adiabatic Mass Loss In Binary Stars. VI. Massive Helium Binary Stars","primary_cat":"astro-ph.SR","submitted_at":"2026-04-07T03:57:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Adiabatic mass-loss models for massive helium stars give critical mass ratios 0.7-3.0 on the main sequence and 1.5-27 on the Hertzsprung gap, lowered by winds and adjusted by isotropic re-emission.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"mal structure out of thermal equilibrium. Here, we use the thermal local timescale to show this mechanism. This timescale represents the time for complete loss of internal energy in the stellar outer envelope using stel- lar luminosity as the power, which can be calculated as follows (R. Kippenhahn et al. 2013), τth (m) = 1 L Z Msurf m Cp (m′)T(m ′) dm′.(2) In this Equation,mrepresents the mass coordinate, Msurf represents the total mass,Lrepresents stellar lu- minosity,C p represents the heat capacity at constant pressure at the specific mass coordinate, andTis the temperature. The local thermal timescales for differ- ent mass-loss rates are shown as the solid lines in the third panel of Figure 5. To reach the limit of local ther-"},{"citing_arxiv_id":"2604.03385","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Deep Adaptive Optics Imaging Rules Out a Helium Star Companion to PSR J1928+1815","primary_cat":"astro-ph.SR","submitted_at":"2026-04-03T18:28:26+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Using stripped-star atmosphere models and conservative extinction estimates, we show that any plausible helium star companion would have been detected, ruling out this interpretation. A massive white dwarf (WD) companion remains consistent with the non-detection. We consider two possible origins for the eclipses: (1) absorption in a wind driven by a young, hot WD, and (2) material ablated from the WD by the pulsar. The former can naturally arise following Case BB mass transfer, which produces∼1.2M ⊙ WDs capable of sustaining winds of ˙M≳10 −12- 10−13 M⊙ yr−1 for∼10 4-105 yr, sufficient to obscure the pulsar at GHz frequencies. The latter requires efficient coupling of the pulsar's spin-down luminosity to the companion to drive the needed"},{"citing_arxiv_id":"2604.02725","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"What Are Pulsar Companions Made of? Using Gravitational Tides to Probe Their Compositions","primary_cat":"astro-ph.HE","submitted_at":"2026-04-03T04:35:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Tidal deformability modeling for pulsar companions enables constraints on their equations of state by matching predicted orbital precession to timing data from four systems.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The boundary condition for this equation isη 2(0) = 0. When calculatingk 2,Love the factor of 1/2can be removed from Equation (6) as seen in J. C. Becker & K. Batygin (2013). Fromk2, we find the tidal deformabilityλof the body, λ= 2R5 3G k2 ,(7) as well as the dimensionless tidal deformability with M=m(R)(T. Hinderer et al. 2010), Λ =k 2 \u0012 Rc2 GM \u00135 = λc10 G4M 5 .(8) Adiscussionofthetidaldeformabilityanddimensionless tidal deformability is provided in Appendix A. 3.2.2.TOV Equations It is necessary to switch from the Hydrostatic Equi- librium equations to the Tolman-Oppenheimer-Volkoff (TOV) equations when studying relativistic internal compositions (J. R. Oppenheimer & G. M. Volkoff 1939; R. C. Tolman 1939). In this regime it becomes much"},{"citing_arxiv_id":"2508.00976","ref_index":14,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Census of Variable Radio Sources at $3\\,$GHz","primary_cat":"astro-ph.GA","submitted_at":"2025-08-01T18:00:00+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A census of ~3600 variable compact radio sources at 3 GHz from VLASS epochs 1 and 2, with 5-9% showing >30% flux changes above 20-300 mJy and most consistent with blazars or quasars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}