{"total":26,"items":[{"citing_arxiv_id":"2605.18731","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2605.17048","ref_index":28,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2605.14447","ref_index":140,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons","primary_cat":"nucl-th","submitted_at":"2026-05-14T06:41:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian analysis finds that the likely ranges of light dark-matter fermion mass and exponential density-profile parameter in hyperon-containing neutron stars are nearly independent of the hadronic model for symmetry-energy slopes between 40 and 58 MeV, with HESS J1731-347 and GW170817 data playing,","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.09206","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Neutron stars in a conservative $f(R,T)$ gravity","primary_cat":"gr-qc","submitted_at":"2026-05-09T22:51:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A conservative f(R,T) gravity reformulation decouples the gravitational sector from the microphysical equation of state, enabling computation of neutron star mass-radius relations and tidal deformabilities that satisfy current astrophysical constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"provide a unique laboratory for probing the properties of dense matter and testing gravitational theories in the strong-field regime. Observations of massive pulsars with masses close to two solar masses [1-4], together with radius measurements from the NICER mission [5- 8] and tidal deformability constraints from gravitational wave observations of binary neutron star mergers [9], have significantly improved our ability to test both the microphysics of dense matter and the underlying theory of gravity. General Relativity has been remarkably successful in describing gravitational phenomena over a wide range of scales. Nevertheless, theoretical and observational motivations continue to drive the exploration of modified theories of gravity [10-12]."},{"citing_arxiv_id":"2605.06418","ref_index":27,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"On the non-radial oscillations of realistic anisotropic neutron stars: Axial modes","primary_cat":"gr-qc","submitted_at":"2026-05-07T15:26:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Axial modes of anisotropic neutron stars show mass-scaled frequency and damping time with nearly universal quadratic dependence on compactness, insensitive to EOS and anisotropy model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"PSR J0030+045 [23, 24] and PSR J0740+662 [25, 26] pro- vide tighter bounds on the permissible anisotropy within a realistic neutron star. Modeling these effects is essential for understanding the behavior of matter under extreme conditions, as anisotropy can stabilize stellar configura- tions that would otherwise be deemed unstable under the assumption of local isotropy [27, 28]. The dynamical response of neutron stars to perturba- tions provides a unique window into their internal com- position, a field known as gravitational-wave asteroseis- mology [29]. Non-radial oscillations are characterized by a spectrum of discrete quasi-normal modes, which are traditionally classified according to their restorative forces: the fundamentalf-mode, pressurep-modes, and"},{"citing_arxiv_id":"2605.05005","ref_index":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Characterizing the quark-hadron mixed phase in compact star cores : sensitivity to nuclear saturation and quark-model parameters at finite-temperature","primary_cat":"nucl-th","submitted_at":"2026-05-06T15:06:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The quark-hadron mixed phase width in hybrid stars is mainly controlled by effective nucleon mass and symmetry energy, with temperature reducing the width and softening the EOS while strong vector repulsion is needed to match massive pulsar and NICER data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"C89, 015806 (2014), arXiv:1308.1657 [nucl- th]. [12] O. E. Nicotra, M. Baldo, G. F. Burgio, and H. J. Schulze, Phys. Rev. D74, 123001 (2006), arXiv:astro-ph/0608021. [13] G. F. Burgio and S. Plumari, Phys. Rev. D77, 085022 (2008), arXiv:0710.5384 [astro-ph]. [14] A. Bhattacharyya, I. N. Mishustin, and W. Greiner, J. Phys. G37, 025201 (2010), arXiv:0905.0352 [nucl-th]. [15] G. Pagliara, M. Hempel, and J. Schaffner-Bielich, Phys. Rev. Lett.103, 171102 (2009), arXiv:0907.3075 [astro- ph.HE]. [16] M. Hempel, G. Pagliara, and J. Schaffner-Bielich, Phys. Rev. D80, 125014 (2009), arXiv:0907.2680 [astro- ph.HE]. [17] N. Yasutake, T. Maruyama, and T. Tatsumi, Phys. Rev. D80, 123009 (2009), arXiv:0910.1144 [nucl-th]. [18] X. Wu and H."},{"citing_arxiv_id":"2605.02467","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Modeling large glitches with core superfluidity in a Hybrid star","primary_cat":"astro-ph.HE","submitted_at":"2026-05-04T11:09:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hybrid star model with core quark pasta pinning superfluid vortices produces glitch amplitudes ΔΩ/Ω of order 10^{-6} matching Vela-like pulsar observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"PSR J1614-2230 PSR J0348+042 PSR J0030+0451 PSR J0740+6620 Gv = 0.3 fm2, B1/4 = 170 MeV Gv = 0.3 fm2, B1/4 = 155 MeV Gv = 0.2 fm2, B1/4 = 170 MeV Gv = 0.2 fm2, B1/4 = 155 MeV FIG. 5. Mass-radius relation of mixed phase EOSs along with the mass and radius constraints.The contours represent con- straints for PSR J0740+6620 [46, 47] and PSR J0030+451 [48, 49]. The horizontal lines indicate radius constraints. The shaded region at the top corresponds to PSR J0952-0607 [50]. III. GLITCH MODEL We consider neutrons inside the star to be in the super- fluid state [11, 14, 51, 52]. Superfluids rotate by forming an array of vortices. A neutron vortex inside the star cannot be considered straight throughout the star with"},{"citing_arxiv_id":"2604.21039","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Conformal prediction for uncertainties in the neutron star equation of state","primary_cat":"nucl-th","submitted_at":"2026-04-22T19:34:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Conformalized quantile regression applied post hoc to neutron star posterior samples yields reliable uncertainty bands validated by empirical coverage studies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20159","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"A Poincar\\'e-covariant study of strange quark stars","primary_cat":"nucl-th","submitted_at":"2026-04-22T03:51:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A Poincaré-covariant vector-vector contact interaction yields an equation of state for strange quark matter whose mass-radius and tidal properties match pulsar and gravitational-wave constraints for two tuned parameter sets.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"dr = 4πr2ϵ(r),(18) whereM(r) is the gravitational mass enclosed within radiusr. Integrating these equations from the center (r= 0) to the surface (r=R, whereP(R) = 0) yields the mass-radius (M−R) relation (MandRare the star's total mass and radius), which can be compared against astrophysical measurements from pulsars such as PSR J0740+6620 [43, 44], PSR J0030+0451 [45, 46], PSR J0437-4715 [47, 48], and the central compact object in HESS J1731-347 [49]. In addition to the mass and radius, gravitational-wave observations (e.g., GW170817) provide stringent con- straints on the tidal deformability of compact stars. The dimensionless tidal deformability Λ characterizes a star's response to an external tidal field and is highly sensitive"},{"citing_arxiv_id":"2604.13208","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Axial Oscillations of Viscous Neutron Stars","primary_cat":"gr-qc","submitted_at":"2026-04-14T18:30:45+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":"(2019), arXiv:1912.05705 [astro-ph.HE]. [3] Thomas E. Rileyet al., \"AN ICERView of PSR J0030+0451: Millisecond Pulsar Parameter Es- timation,\" Astrophys. J. Lett.887, L21 (2019), arXiv:1912.05702 [astro-ph.HE]. [4] M. C. Milleret al., \"The Radius of PSR J0740+6620 from NICER and XMM-Newton Data,\" Astrophys. J. Lett.918, L28 (2021), arXiv:2105.06979 [astro-ph.HE]. [5] Thomas E. Rileyet al., \"A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy,\" Astrophys. J. Lett.918, L27 (2021), arXiv:2105.06980 [astro-ph.HE]. [6] Slavko Bogdanov, George B. Rybicki, and Jonathan E. Grindlay, \"Constraints on Neutron Star Properties from X-ray Observations of Millisecond Pulsars,\" Astrophys."},{"citing_arxiv_id":"2604.13011","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Buchdahl Limit and TOV Equations in Interacting Vacuum Scenarios","primary_cat":"gr-qc","submitted_at":"2026-04-14T17:46:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Interacting vacuum energy relaxes the pressure gradient inside stars, allowing finite central pressure and compactness beyond the Buchdahl bound for suitable coupling strengths.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"of the art in this field has been significantly reshaped by high-precisio n observations from the Laser Interferometer Gravitational-Wave Observatory (LIGO) and the Neutron Star In terior Composition Explorer (NICER). Through the detection of binary neutron star mergers[4] and the precise mapp ing of pulsar mass-radius relations for both canonical and high-mass sources[5, 6], these missions have provided unprece dented constraints on the neutron star equation of state (EoS), necessitating a rigorous re-evaluation of classical s tability limits in the high-density regime. Despite the remarkable success of General Relativity, the nature of dark energy and the mechanism driving late-time cosmic acceleration remain among the most significant challenges in mo dern physics."},{"citing_arxiv_id":"2604.11046","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Sensitivity of Neutron Star Observables to Transition Density in Hybrid Equation-of-State Models","primary_cat":"nucl-th","submitted_at":"2026-04-13T06:22:40+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(LIGO Scientific, Virgo), Astrophys. J. Lett.882, L24 (2019), arXiv:1811.12940 [astro-ph.HE] . [27] D. Choudhuryet al., Astrophys. J. Lett.971, L20 (2024), arXiv:2407.06789 [astro-ph.HE] . [28] L. Mauviardet al., Astrophys. J.995, 60 (2025), arXiv:2506.14883 [astro-ph.HE] . 7 [29] T. E. Rileyet al., Astrophys. J. Lett.887, L21 (2019), arXiv:1912.05702 [astro-ph.HE] . [30] M. C. Milleret al., Astrophys. J. Lett.887, L24 (2019), arXiv:1912.05705 [astro-ph.HE] . [31] T. E. Rileyet al., Astrophys. J. Lett.918, L27 (2021), arXiv:2105.06980 [astro-ph.HE] . [32] M. C. Milleret al., Astrophys. J. Lett.918, L28 (2021), arXiv:2105.06979 [astro-ph.HE] . [33] M. Punturoet al., Class. Quant. Grav.27, 194002 (2010). [34] D. Reitzeet al."},{"citing_arxiv_id":"2604.04560","ref_index":64,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Neutron star with dark matter using vector portal","primary_cat":"hep-ph","submitted_at":"2026-04-06T09:40:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Vector portal fermionic dark matter admixed in neutron stars produces mediator-mass-dependent changes to the equation of state, yielding distinct mass-radius relations and tidal deformabilities that observations can use to constrain the model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"gqZ ′ ≃1/3g N Z′) is taken to be same as the couplingg χZ′ of the DM with the vector boson Z′ [97, 98]. In set 1, we have taken a heavyZ ′ with mass around 1800 GeV along with the DM massm χ ≃200 GeV. The set 2 corresponds to a larger DM massm χ ≃1800 GeV and mZ′ ≃900 GeV. These are the limiting cases for the parameters satisfying relic density, direct detection and dijet bounds from collider studies [64]. The set 3 corresponds to a light vector mediator (Z ′) which is inspired by the experiments on rare semi-leptonic decays of b→sℓℓtransition [99]. For the nuclear matter EOS, we use the RMF model as in Eq. (2.1) with a parameterization considered recently in Ref. [100] obtained by using a Bayesian analysis. This parameter set for the RMF model is given in Table 2 and corresponding"},{"citing_arxiv_id":"2604.02782","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Spin effects in superfluidity, neutron matter and neutron stars","primary_cat":"astro-ph.HE","submitted_at":"2026-04-03T06:47:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review of spin effects, superfluidity, and magnetic fields in neutron matter and their influence on neutron-star structure, superfluid phases, and rotational dynamics.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Abraham, F. Acernese, K. Ackley et al.,GW190425: Observation of a Compact Binary Coalescence with Total Mass∼ 3.4 M ⊙,Astrophys. J. Lett.892(2020) L3, [2001.01761]. [19] E. E. Flanagan and T. Hinderer,Constraining neutron-star tidal love numbers with gravitational-wave detectors,Phys. Rev. D-Particles, Fields, Gravitation, and Cosmology77(2008) 021502. [20] T. Hinderer,Tidal Love numbers of neutron stars, Astrophys. J.677(2008) 1216-1220, [0711.2420]. [21] T. E. Riley, A. L. Watts, S. Bogdanov et al.,A N ICERView of PSR J0030+0451: Millisecond Pulsar Parameter Estimation,Astrophy. J. Lett.887 (2019) L21, [1912.05702]. [22] M. C. Miller, F. K. Lamb, A. J. Dittmann et al.,PSR J0030+0451 Mass and Radius fromN ICERData and"},{"citing_arxiv_id":"2601.07931","ref_index":40,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly","primary_cat":"gr-qc","submitted_at":"2026-01-12T19:01:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Roughly half of realistic neutron-star equations of state produce stars with negative Ricci scalar inside, and an improved analytic fit links gravitational mass M to baryonic mass Mb with maximum 3 percent variance.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.24194","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Impact of Anisotropy on Neutron Star Structure and Curvature","primary_cat":"gr-qc","submitted_at":"2025-12-30T12:53:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl scalar stays largely insensitive.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.02484","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Properties of Stable Massive Quark Stars in Holography","primary_cat":"hep-ph","submitted_at":"2025-12-02T07:18:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Holographic model of massive deconfined quarks yields a stiff enough equation of state to allow stable 2-solar-mass hybrid stars with quark cores for certain nuclear phases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.20477","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Rotational effects in quark stars: comparing different models","primary_cat":"astro-ph.HE","submitted_at":"2025-11-25T16:41:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Rotation amplifies differences between the vector MIT bag and DDQM equations of state for quark stars, with MIT supporting more massive stars and a full decomposition of gravitational, internal, rotational, and binding energies provided.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.19626","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Universal Relations with Dynamical Tides","primary_cat":"gr-qc","submitted_at":"2025-11-24T19:01:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"New quasi-universal relations connect static tidal deformability Λ⁰ to its dynamical correction Λ² and to Mω* with equation-of-state scatter below 5% and 2.8% respectively across 59 models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.07567","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach","primary_cat":"astro-ph.HE","submitted_at":"2025-11-10T19:22:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dark matter cores heat baryonic matter in evolving proto-neutron stars by deepening the gravitational potential while halos cool it, providing a diagnostic distinct from hyperons.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.07226","ref_index":54,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Renormalization-Group Invariant Parity-Doublet Model for Nuclear and Neutron-Star Matter","primary_cat":"nucl-th","submitted_at":"2025-11-10T15:46:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A renormalization-group invariant mean-field treatment of the Parity-Doublet Model is developed that consistently includes baryonic vacuum fluctuations and is used to study chiral symmetry restoration in two-flavor nuclear and neutron-star matter for chosen values of the chirally invariant mass m0.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.06489","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Sub-GeV dark matter in neutron stars: halo morphologies and their suppression by vacuum-like pressure","primary_cat":"astro-ph.HE","submitted_at":"2025-11-09T18:25:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A small vacuum-like dark-energy admixture in neutron stars with 400 MeV–1 GeV fermionic dark matter shrinks halo-induced radius differences from several kilometers to sub-kilometer scales and mass differences to ≲1%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.06145","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Equation of State Extrapolation Systematics: Parametric vs. Nonparametric Inference of Neutron Star Structure","primary_cat":"astro-ph.HE","submitted_at":"2025-09-07T17:21:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Nonparametric GP-based high-density extensions yield softer EOS posteriors with larger uncertainties than parametric PP extensions when jointly constrained by multi-messenger neutron star observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.05564","ref_index":60,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bayesian Inference of the Landau Parameter $G'_0$ from Joint Gamow-Teller Measurements","primary_cat":"nucl-th","submitted_at":"2025-06-05T20:19:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bayesian inference from joint GTR measurements on 208Pb, 132Sn, and 90Zr yields G'_0 = 0.48 ± 0.034 in a standard Skyrme RPA framework.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2504.18764","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Symmetry Energy Expansion with Strange Dense Matter","primary_cat":"nucl-th","submitted_at":"2025-04-26T01:56:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A redefinition of the symmetry energy expansion that incorporates finite strangeness consistent with SU(3) flavor symmetry and remains valid beyond typical neutron-star central densities.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2409.10508","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars","primary_cat":"astro-ph.HE","submitted_at":"2024-09-16T17:54:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Resistive GRMHD simulations of rotating neutron stars show resistivity changes magnetic field geometries, suppresses instabilities, and lowers GW emission amplitude while maintaining a consistent 9:1 poloidal-to-toroidal energy ratio over 100 ms.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Riley, A. L. Watts, S. Bogdanov, P. S. Ray, R. M. 18 Ludlam, S. Guillot, Z. Arzoumanian, C. L. Baker, A. V. Bilous, D. Chakrabarty, K. C. Gendreau, A. K. Hard- ing, W. C. G. Ho, J. M. Lattimer, S. M. Morsink, and T. E. Strohmayer, A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation, ApJ 887, L21 (2019), arXiv:1912.05702 [astro-ph.HE]. [9] A. V. Bilous, A. L. Watts, A. K. Harding, T. E. Riley, Z. Arzoumanian, S. Bogdanov, K. C. Gendreau, P. S. Ray, S. Guillot, W. C. G. Ho, and D. Chakrabarty, A NICER View of PSR J0030+0451: Evidence for a Global-scale Multipolar Magnetic Field, ApJ 887, L23 (2019), arXiv:1912.05704 [astro-ph.HE]. [10] R. C. R. de Lima, J. G. Coelho, J. P. Pereira, C."}],"limit":50,"offset":0}