{"total":15,"items":[{"citing_arxiv_id":"2605.23021","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Finite-Size Effects on the Critical End Point of Magnetized Quark Matter in the Nonlocal PNJL Model","primary_cat":"hep-ph","submitted_at":"2026-05-21T20:45:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Finite-size effects in the nonlocal PNJL model shift the critical end point of magnetized quark matter toward higher chemical potentials and lower temperatures as droplet radius decreases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20632","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multi-wavelength Emission for a Post-merger Magnetar: The Magnetar-Driven Poynting Jet and Its Associated Pulsar Wind Nebula","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T02:36:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A dynamical model of magnetar-driven jet and PWN emission predicts a sequence of thermal, X-ray plateau, and late synchrotron/inverse-Compton radiation that accounts for key features in merger GRBs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17438","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Holographic entanglement entropy in the QCD phase diagram under external magnetic field","primary_cat":"hep-th","submitted_at":"2026-05-17T13:20:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Holographic entanglement entropy exhibits a swallow-tail structure indicating connected-to-disconnected transitions for perpendicular magnetic fields in the QCD phase diagram while remaining monotonic for parallel fields, consistent with black hole thermodynamics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17048","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Nonlinear electrodynamics in magnetars: systematic effects on radius constraints and timing analysis","primary_cat":"astro-ph.HE","submitted_at":"2026-05-16T15:40:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"NLED alters photon propagation near magnetars, producing ~10% errors in inferred radii via ray-tracing and a minimal ~350 ns travel-time delay.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07255","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Resonant Inverse Compton Scattering and Hard X-ray Emission in Magnetar Magnetospheres","primary_cat":"astro-ph.HE","submitted_at":"2026-05-08T05:23:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Equatorial twist geometry in the magnetar magnetosphere allows resonant Compton upscattering to reproduce the hard X-ray spectrum of 4U 0142+61 with optical depth limits from resonant cooling.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We first integrate the scattering rate over the azimuthal angleϕwith respect to the magnetic axis to exploit theδ(x ′ −b) function in Equation (8). Therefore, dNp→q dt dxf dΩf drmaxdθ (xf , rmax, θ,Ω f) = Z dϕ ner2 max sin7 θ ×R3 NS c γ2(1−βµ f) Z dΩi dn dxidΩi σeffPp→q X ϕres δ(g(ϕ)) |g′(ϕ)| = X ϕres ner2 max sin7 θR3 NS cσeff γ2(1−βcosθ f) 1 |g′(ϕ)| × Z dΩi dn dxidΩi Pp→q. (10) Here we adopt the Jacobian of the volume integration dV=r 2 max sin7 θR3 NSdrmaxdθdϕ, and define g(ϕ) =x f γ(1−βµ f)−b.(11) Alternatively, we can use the field loop footpoint co- latitudeθ foot instead ofr max, and the volume element dV=r 3 sinθ foot cosθ footR3 NSdrdθfootdϕ/cosθ. The out- going scattering angleµ f can be related to the scatter- ing locale (r max, θ, ϕ) and the viewing colatitude with"},{"citing_arxiv_id":"2605.00720","ref_index":159,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A bright wideband radio burst from the isolated neutron star 2XMM J104608.7$-$594306","primary_cat":"astro-ph.HE","submitted_at":"2026-05-01T15:08:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A second coherent radio burst spanning 704-4032 MHz with spectral index -2.18, 54% linear and 22% circular polarization, and an orthogonal polarization angle jump was detected from 2XMM J104608.7-594306, showing rare radio activity in sources thought to be radio-quiet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.26715","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Thermodynamics of magnetized matter in hot and dense QCD","primary_cat":"hep-lat","submitted_at":"2026-04-29T14:20:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"A pedagogical review of lattice QCD results on the thermodynamics of hot, dense, and magnetized QCD matter with an outlook on open questions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"While the baryon density is typically dominant, there might be physical systems where the charge density governs the properties of the system, such as in the early Universe in the presence of large lepton flavor asymmetries [1]. In addition to non-zero temperature and density, the aforementioned systems can also feature electromagnetic fields with magnitudes comparable to the QCD scale. These are expected to be present in the core of magnetars [2], magnetized neutron stars, in off-central HICs [3], and might have been created at early times during the evolution of the Universe [4] prior to the QCD transition. Electromagnetic fields of this magnitude strongly affects the quarks and, through them, the thermodynamic properties of strongly interacting matter. For a consistent phenomenological treatment, the effects of these fields therefore has to be taken into account."},{"citing_arxiv_id":"2604.24750","ref_index":9,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spectral Evidence of Heavy Nuclei from the Neutron Star Crust in Magnetar Bursts","primary_cat":"astro-ph.HE","submitted_at":"2026-04-27T17:54:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Spectral fits to magnetar burst X-rays disfavor light ions and favor effective charge Z~37, providing evidence for heavy nuclei from the neutron star crust.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The normalization con- stantn c =e −µc is directly related to the total number of photons in the distribution (S. K. Acharya et al. 2021). 2.3.Observed flux spectrum The intensity considering absorption, coherent scat- tering, and inverse Compton effects may be estimated as (G. B. Rybicki & A. P. Lightman 1986), Iν =I E ν +I W ν =I ν(ν, kT, B, n e, Z, A, θ). (9) Assuming the photons are isotropic before and after scattering, the differential number dNor the probabil- ity dN/Nof photons in an interval (θ, θ+ dθ) can be expressed as, dN/N=f(θ) = dΩ/Ω = sinθdθ/2,(10) Therefore, we have, Iν = Z π 0 f(θ)·I ν(θ) =I ν(ν, kT, B, n e, Z, A). (11) The observed fluxF ν [erg cm −2 s−1 Hz−1] spectrum is then calculated by,"},{"citing_arxiv_id":"2604.22680","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dense Matter and Compact Stars in Strong Magnetic Fields","primary_cat":"astro-ph.HE","submitted_at":"2026-04-24T16:02:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Strong magnetic fields in compact stars induce Landau quantization and magnetic-moment couplings that change the equation of state and allow additional degrees of freedom such as hyperons, Delta resonances, and quark matter.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"A significant fraction of SGR and AXP sources are found in association with supernova remnants, supporting their identification as NSs. These objects are generally considered to be relatively young and are characterized by comparatively long spin periods. The emission from these sources is widely interpreted as originating from the release of magnetic energy stored in the stellar interior [4,7] with surface magnetic field ∼ 1015 − 1016 G, as estimated from spin-down measurements, are classified asmagnetars [20,21]. Figure 1. P˘ ˙P diagram of the observed pulsar population. Dashed curves indicate lines of constant characteristic age and surface magnetic field. Binary pulsars, RAdio Transients (RRATs), and magne- tars are shown as circles, stars, and upward triangles, respectively."},{"citing_arxiv_id":"2604.20814","ref_index":199,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Search for Rotation Measure Flare Candidates in Repeating Fast Radio Bursts","primary_cat":"astro-ph.HE","submitted_at":"2026-04-22T17:44:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A search of repeating FRBs identifies RM flare candidates in FRB 20121102A, FRB 20201124A, and FRB 20180916B, suggesting such events may be common and tied to dynamic magneto-ionic environments.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19497","ref_index":104,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Design and preliminary performance study of the broad-band spectrometer detector for POLAR-2","primary_cat":"astro-ph.IM","submitted_at":"2026-04-21T14:18:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations of the BSD instrument for POLAR-2 show it can localize faint GRBs like GRB 170817A to about 1.5 degrees accuracy, meeting requirements for supporting GRB polarimetry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.07734","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Resolving the 2024 Outburst of Magnetar 1E 1841-045 from its host Supernova Remnant with EP-FXT","primary_cat":"astro-ph.HE","submitted_at":"2026-04-09T02:31:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New EP-FXT data on the 2024 outburst of magnetar 1E 1841-045 shows energy-dependent multi-peaked pulses, spectral hardening, BB temperature-pulse intensity correlations, and effective separation from supernova remnant emission.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.08119","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Impact of Resonant Compton Scattering on Magnetar X-Ray Polarization with QED Vacuum Resonance","primary_cat":"astro-ph.HE","submitted_at":"2026-03-09T08:59:51+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":"2601.15452","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The long quest for vacuum birefringence in magnetars: 1E 1547.0-5408 and the elusive smoking gun","primary_cat":"astro-ph.HE","submitted_at":"2026-01-21T20:35:49+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"IXPE data on magnetar 1E 1547.0-5408 show high linear polarization from a small hot spot whose phase-dependent angle is fit by a rotating vector model, with a marginal energy-dependent dip in polarization degree that may indicate vacuum resonance but does not constitute compelling evidence for biref","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.10239","ref_index":61,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"EP250827b/SN 2025wkm: An X-ray Flash-Supernova Powered by a Central Engine and Circumstellar Interaction","primary_cat":"astro-ph.HE","submitted_at":"2025-12-11T02:44:47+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"EP250827b/SN 2025wkm is an X-ray flash supernova at z=0.1194 powered by a long-lived magnetar and disk winds interacting with extended circumstellar medium, without an on-axis relativistic jet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}