{"total":12,"items":[{"citing_arxiv_id":"2605.18731","ref_index":152,"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":"2605.14264","ref_index":101,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The compact neutron star in 4U 1746-37 revisited: Reassessing the mass and radius","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T02:08:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Significant X-ray flux blocking in 4U 1746-37 allows the neutron star to have canonical mass and radius values of 1.59 solar masses and 13 km or 2.12 solar masses and 9.8 km.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.09206","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Arzoumanian, H. Blumer, P. R. Brook, S. Burke-Spolaor, S. J. Chamberlin, S. Chatterjee, J. M. Cordes, R. D. Ferdman, W. Fiore, N. Garver-Daniels, P. A. Gentile, J. W. T. Hessels, G. Jones, M. T. Lam, D. R. Lorimer, R. S. Lynch, M. A. McLaughlin, T. T. Pennucci, I. H. Stairs, K. Stovall, J. Swiggum, and W. W. Zhu, Nature Astronomy4, 72 (2020), 1904.06759. [4] E. Fonseca, H. T. Cromartie, T. T. Pennucci, P. S. Ray, A. Y. Kirichenko, S. M. Ransom, P. B. Demorest, I. H. Stairs, Z. Arzoumanian, H. Blumer, P. R. Brook, S. Burke-Spolaor, S. Chatterjee, J. M. Cordes, T. Enoto, W. Fiore, P. A. Gentile, D. C. Good, J. L. Han, J. W. T. Hessels, R. J. Jennings, G. Jones, M. T. Lam, T. J. W. Lazio, D. R. Lorimer, R."},{"citing_arxiv_id":"2604.04560","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Axion-Like-Particles,JHEP01(2019) 163, [arXiv:1807.10773]. [53] J.-F. Fortin and K. Sinha,Constraining Axion-Like-Particles with Hard X-ray Emission from Magnetars,JHEP06(2018) 048, [arXiv:1804.01992]. [54] C. H. Lenzi, M. Dutra, O. Louren¸ co, L. L. Lopes, and D. P. Menezes,Dark matter effects on hybrid star properties,Eur. Phys. J. C83(2023), no. 3 266, [arXiv:2212.12615]. [55] C. Kouvaris and P. Tinyakov,Can Neutron stars constrain Dark Matter?,Phys. Rev. D82 (2010) 063531, [arXiv:1004.0586]. [56] H. Sotani and A. Kumar,Universal relation involving fundamental modes in two-fluid dark matter admixed neutron stars,Eur. Phys. J. C85(2025), no. 12 1438, [arXiv:2512.07105]. [57] A. Issifu, P. Thakur, D. Rafiei Karkevandi, F."},{"citing_arxiv_id":"2604.02782","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Tolman,Static solutions of einstein's field equations for spheres of fluid,Phys. Rev.55(1939) 364-373. [8] J. R. Oppenheimer and G. M. Volkoff,On massive neutron cores,Phys. Rev.55(1939) 374-381. [9] L. D. Landau and E. M. Lifshitz,Statistical physics, Part 1. Pergamon Press, New York, 1980. [10] I. I. Shapiro,Fourth test of general relativity,Phys. Rev. Lett.13(1964) 789-791. [11] P. Demorest, T. Pennucci, S. Ransom, M. Roberts and J. Hessels,Shapiro Delay Measurement of A Two Solar Mass Neutron Star,Nature467(2010) 1081-1083, [1010.5788]. [12]NANOGravcollaboration, Z. Arzoumanian et al., The NANOGrav 11-year Data Set: High-precision timing of 45 Millisecond Pulsars,Astrophys. J. Suppl. 235(2018) 37, [1801.01837]. [13] H. T."},{"citing_arxiv_id":"2602.02272","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Radial Oscillations of Neutron Stars with Vector-Induced Scalar Hair","primary_cat":"gr-qc","submitted_at":"2026-02-02T16:13:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In scalar-vector-tensor gravity, the vector-curvature coupling alters neutron star mass-radius curves and radial oscillation frequencies while preserving the coincidence of maximum mass with the onset of radial instability.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.02484","ref_index":12,"ref_count":1,"confidence":0.98,"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":"2510.22137","ref_index":32,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inferring neutron-star Love-Q relations from gravitational waves in the hierarchical Bayesian framework","primary_cat":"gr-qc","submitted_at":"2025-10-25T03:18:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Hierarchical Bayesian inference on 20 high-SNR simulated binary neutron star events shows a linear lnΛ-lnQ relation suffices and constrains dynamical Chern-Simons gravity length scale to ≤10 km.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.13322","ref_index":76,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities","primary_cat":"hep-ph","submitted_at":"2025-09-16T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Analytical expressions for ALP-photon conversion in transient compact stars yield an updated bound g_aγ < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV from SN 1987A, plus sensitivity forecasts for future Galactic SN and NSM observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The two lighter cases are also the cooler ones, each reaching maximum temperatures of around 40 MeV. In contrast, the heavier models reach up to 60 MeV and are therefore representative of the hotter end of the spectrum. In the model names, numbers such as 18.8 denote the progenitor star's mass in solar units. - 17 - The first letters of the model names denote the used EoS. The SFHo one [76] is fully compatible with all current constraints from nuclear theory and experiment [77-79] as well as astrophysics, including pulsar mass measurements [80-82] and the radius constraints deduced from gravitational-wave and Neutron Star Interior Composition Explorer mea- surements [83-85]. Results for the long-used LS220 EoS [86] are shown for comparison."},{"citing_arxiv_id":"1907.04654","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Phase transitions in neutron stars and their links to gravitational waves","primary_cat":"astro-ph.HE","submitted_at":"2019-07-05T19:07:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review of neutron star dense matter, hadron-quark phase transitions, and potential g-mode signatures in gravitational waves from multimessenger observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Besides the two NSs involved in GW170817, there are about 40 NSs with estimated masses 2. Some of them are extremely precisely determined from their orbital parameters. NSs masses tend to concentrate around the canonical 1.4 M ⊙ but the most stringent observational constraints on the NS EoS arise from two pulsating NSs in binary systems with white dwarfs companions: PSR J1614-2230 [13] with M = 1.908± 0.016 M ⊙ [16], and PSR J0348+0432, with M = 2.01± 0.04 M⊙ [15]. These highly precise measurements based on timing analysis, challenge the high-density EoS models, but also impose limits on the EoS at lower densities (see figure 6 in section 5). On the other hand, NSs spin can be precisely determined either from pulsar radio or X-ray timing obser-"},{"citing_arxiv_id":"1907.06597","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hot quark matter and (proto-) neutron stars","primary_cat":"nucl-th","submitted_at":"2019-07-05T16:10:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"An extended PNJL model locates the QCD critical end point and predicts that proto-neutron stars contain hyperons and Delta-isobars but no deconfined quarks, which appear only in cold neutron stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.03549","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Anisotropic strange quark stars with a non-linear equation-of-state","primary_cat":"gr-qc","submitted_at":"2019-07-05T10:16:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Exact analytical solution for anisotropic CFL strange quark stars with non-linear EOS, satisfying energy conditions, yielding mass-radius profiles and compactness values.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}