{"total":39,"items":[{"citing_arxiv_id":"2606.23602","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Data analysis methods for powder x-ray diffraction intensity under laser-driven dynamic compression at Omega and NIF laser facilities","primary_cat":"cond-mat.mtrl-sci","submitted_at":"2026-06-22T17:05:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Develops methods for accurate PXRD intensity measurement under dynamic compression using in-situ references from pinholes or uncompressed material and corrections for thermal damping, illustrated on diamond near 1 TPa.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09247","ref_index":72,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bayesian analysis of the shear modulus in the neutron-star crust","primary_cat":"astro-ph.HE","submitted_at":"2026-06-08T09:20:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.30548","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Magnetic Eruption and Nucleosynthesis in GR{\\nu}MHD Simulations of Spinning Neutron Star Mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-05-28T20:30:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"3D GRMHD simulations with second-moment neutrino transport show aligned spins produce more collimated polar outflows and 2.4e-3 solar masses of proton-rich material yielding light r-process elements like 56Ni, while antialigned spins disrupt magnetic amplification.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28944","ref_index":95,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of the equation of state on core collapse supernovae I: the low-$T/|W|$ instability","primary_cat":"astro-ph.HE","submitted_at":"2026-05-27T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21640","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Wave Hyperbolic Catalog: Reanalyzing High-Mass Gravitational Wave Signals Using Hyperbolic Waveforms","primary_cat":"gr-qc","submitted_at":"2026-05-20T18:51:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reanalysis finds GW190521 prefers hyperbolic waveforms over quasi-circular precessing ones with ln Bayes factor 3.71, while other high-mass events and GW231123 favor the latter; mock signals indicate distinguishability challenges for high-mass precessing cases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16132","ref_index":54,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nucleosynthesis in the fast ejecta of a neutron star merger","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T16:15:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14447","ref_index":37,"ref_count":1,"confidence":0.98,"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":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Following our previous works [37-39, 48], in the present work the values ofmχ,m η andm ξ are consistently related with the self-interaction constraints from bullet cluster [40-44] while the self-interaction couplingsy η andy ξ are also chosen by reproducing the observed non-baryonic relic density [45-47]. The permitted values ofm η andm ξ corresponding to the range ofm χ are already shown in our previous works [37, 38, 48]. The direct detection, indirect detection, and collider search avenues for DM have excluded a vast region of the DM-SM interaction parameter space (SM stands for the standard model particles). Of late, light DM of mass in the sub-GeV order, has garnered a lot of attention. Therefore, in this work, we particularly focus on them χ ≤1 GeV domain to understand the possible existence of"},{"citing_arxiv_id":"2605.13036","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inspiral gravitational waveforms from charged compact binaries with scalar hair","primary_cat":"gr-qc","submitted_at":"2026-05-13T05:44:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In Einstein-scalar-Maxwell theories, charged compact binaries produce gravitational waveforms containing a leading -1 post-Newtonian dipole correction controlled by one deviation parameter b.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"848, L13 (2017), arXiv:1710.05834 [astro-ph.HE]. [6] B. P. Abbottet al.(LIGO Scientific, Virgo),Phys. Rev. Lett.121, 161101 (2018), arXiv:1805.11581 [gr-qc]. [7] P. Creminelli and F. Vernizzi,Phys. Rev. Lett.119, 251302 (2017), arXiv:1710.05877 [astro-ph.CO]. [8] J. M. Ezquiaga and M. Zumalacarregui,Phys. Rev. Lett.119, 251304 (2017), arXiv:1710.05901 [astro-ph.CO]. [9] J. Sakstein and B. Jain,Phys. Rev. Lett.119, 251303 (2017), arXiv:1710.05893 [astro-ph.CO]. [10] T. Baker, E. Bellini, P. G. Ferreira, M. Lagos, J. Noller, and I. Sawicki,Phys. Rev. Lett.119, 251301 (2017), arXiv:1710.06394 [astro-ph.CO]. [11] R. Kase and S. Tsujikawa,Int. J. Mod. Phys. D28, 1942005 (2019), arXiv:1809.08735 [gr-qc]. [12] R. 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Poisson, Physical Review D80, 084018 (2009), 0906.1366."},{"citing_arxiv_id":"2605.08584","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover","primary_cat":"astro-ph.HE","submitted_at":"2026-05-09T01:00:23+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"structures found in the posterior EOS are driven solely by physical conditions rather than by mathematically distorted priors. Finally, in the Bayesian analysis, we combine several observational constraints to evaluate these physically unbi- ased EOS samples. We incorporate the NICER mass-radius constraints for PSR J0030+0451 [3] in ST+PDT model- ing, PSR J0740+6620 [4], PSR J0437−4715 [6], and PSR J0614−3329 [7], the GW170817 mass-tidal-deformability posterior [1], and the pulsar-mass constraints that enter through the two-solar-mass requirement. Results.The reconstructed posteriors of the EOS, extending continuously from the low-densityχEFT region to the high- density pQCD limit atµ B =2.6 GeV , are shown in Fig."},{"citing_arxiv_id":"2605.08569","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Good, the Bad, and the Subtle: Relativistic mode sums for neutron-star tidal response","primary_cat":"gr-qc","submitted_at":"2026-05-09T00:04:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A practical relativistic mode-sum method for neutron-star tidal response is implemented, with robust f-mode agreement to direct matching but acknowledged limitations in convergence and tidal field uniqueness.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"D80, 084018 (2009), arXiv:0906.1366 [gr-qc]. [6] Thibault Damour and Alessandro Nagar, \"Relativistic tidal properties of neutron stars,\" Phys. Rev. D80, 084035 (2009), arXiv:0906.0096 [gr-qc]. [7] S. Chandrasekhar, \"A General Variational Principle Gov- erning the Radial and the Non-Radial Oscillations of Gaseous Masses.\" Astrophys. J.139, 664 (1964). [8] D. Lynden-Bell and J. P. Ostriker, \"On the stability of differentially rotating bodies,\" Monthly Notices of the Royal Astronomical Society136, 293 (1967). [9] J. L. Friedman and B. F. Schutz, \"Lagrangian perturba- tion theory of nonrelativistic fluids.\" Astrophys. J.221, 937-957 (1978). [10] W. H. Press and S. A. Teukolsky, \"On formation of close"},{"citing_arxiv_id":"2605.05005","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"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. Shen, Phys. Rev. C96, 025802 (2017), arXiv:1708.01878 [nucl-th]. [19] A. Steiner, M. Prakash, and J. M. Lattimer, Phys. Lett. B486, 239 (2000), arXiv:nucl-th/0003066. [20] G. Pagliara, M. Hempel, and J. Schaffner-Bielich, Physical Review Letters103(2009), 10.1103/phys- revlett.103.171102. [21] N. K. Glendenning, Phys. Rept.342, 393 (2001)."},{"citing_arxiv_id":"2604.25107","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Large amplification of the isospin-dependence of proton emitting source size in radioactive heavy-ion collisions: a signal of n-p correlation","primary_cat":"nucl-ex","submitted_at":"2026-04-28T01:28:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Proton emitting source size is amplified by 24% in neutron-rich versus neutron-deficient tin collisions, revealing a beyond-mean-field short-range n-p correlation effect.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"neutron-star matter, including associated phenomena such as neutrino and gravitational-wave emission [ 11, 12]. Focusing on tin isotopes, the ground-state charge radius of 132Sn differs from that of 108Sn by only about 3% [ 1, 2], con- sistent with mean-field expectations. Theoretical studies have shown that 𝑛𝑝 correlations around the Fermi surface shape charge radius systematics across closed shells [ 13]. If the collision dynamics simply reflected the ground-state distribu- tions, one would expect a similarly modest difference in the proton emitting source size between neutron-rich and neutron- deficient systems. However, the dynamics of a HIC may am- plify correlations that are mild in the ground state. Transport models that incorporate the neutron skin and mean-field dy-"},{"citing_arxiv_id":"2604.24949","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Physics Informed Bayesian Neural Network for the Neutron Star Equation of State","primary_cat":"astro-ph.HE","submitted_at":"2026-04-27T19:48:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A physics-informed Bayesian neural network learns neutron-star equations of state from theoretical priors and constraints, then generates posterior mass-radius and mass-tidal-deformability distributions consistent with NICER radii and 2-solar-mass limits.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Lett.120, 172703 (2018), 1711.02644. [9] J. Antoniadiset al., Science340, 6131 (2013), 1304.6875. [10] H. T. Cromartieet al.(NANOGrav), Nature Astron.4, 72 (2019), 1904.06759. [11] E. Fonsecaet al., Astrophys. J. Lett.915, L12 (2021), 2104.00880. [12] A. W. Steiner, J. M. Lattimer, and E. F. Brown, The Astrophysical Journal722, 33 (2010), 1005.0811. [13] P. Landry, R. Essick, and K. Chatziioannou, Physical Review D101, 123007 (2020), 2003.04880. [14] G. Raaijmakerset al., The Astrophysical Journal Letters 918, L29 (2021), 2105.06981. [15] K. Zhouet al., Progress in Particle and Nuclear Physics 135, 104084 (2024), 2303.15136. [16] G. Papigkiotiset al., Physical Review D111, 083056 (2025), 2501.18544."},{"citing_arxiv_id":"2604.21990","ref_index":44,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A New Spin on Dissipative Tides: First-Post-Newtonian Effects in Compact Binary Inspirals","primary_cat":"gr-qc","submitted_at":"2026-04-23T18:17:29+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":"unclear","context_text":"two deformable bodies undergoing conservative tidal in- teractions, and then computed the resulting waveform in [43]. Such an analysis was recently extended to bi- nary neutron stars by HRY [26] in their investigations of dissipative tidal effects. Higher-order corrections to the adiabatic tidal waveform due to spin-tidal couplings were computed in [44], who also used the formalism of [31, 41]. More recently, EFT methods have been used to model tidal interactions, with works such as [23, 32, 45- 47]usingaworldlineeffectiveactionformalism, andthose 4 such as [39, 42, 48-50] using diagrammatic methods. Let us proceed by considering the dynamics of a bi- nary system composed of two deformable bodies."},{"citing_arxiv_id":"2604.21859","ref_index":20,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mitigating Systematic Errors in Parameter Estimation of Binary Black Hole Mergers in O1-O3 LIGO-Virgo Data","primary_cat":"astro-ph.HE","submitted_at":"2026-04-23T16:52:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reanalysis of flagged LVK events with waveform uncertainty models produces consistent spin and precession inferences across raw/deglitched data and multiple waveform approximants.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"improves, waveform models need to catch up with the re- quired accuracy [52]. A given waveform model may suffer from inaccuracies due to the modeling ansatz [53, 54], un- certainties in the numerical relativity calibration schemes [55, 56], or the extrapolation of calibration schemes into regions of parameter space where only a few numerical relativity simulations are available [20]. In the literature, many schemes are proposed and employed to account for arXiv:2604.21859v1 [astro-ph.HE] 23 Apr 2026 2 waveform systematic uncertainties [57]. Some of these schemes fall into the category of accounting for system- atic differences across waveform models: either by mixing posterior samples from multiple PE runs [58-60] or by as-"},{"citing_arxiv_id":"2604.14134","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"All-order structure of static gravitational interactions and the seventh post-Newtonian potential","primary_cat":"hep-th","submitted_at":"2026-04-15T17:55:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A closed formula computes static post-Newtonian corrections at arbitrary odd orders in gravity, yielding the explicit seventh post-Newtonian potential that matches an independent diagrammatic method.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"It underlies the generation of gravita- tional waves (GWs), which encode information about the internal structure of compact objects before and after coalescence. Precise theoretical predictions for such sys- tems offer a unique opportunity to understand the distri- butions of black hole masses and spins [1], constraints on the neutron-star equation-of-state [2], measurements of the Hubble-Lemaˆ ıtre parameter [3-5], and constraints on the theory of General Relativity (GR) [6-9]. Systematic biases are already visible in the current gravitational- wave analyses [10-12], which call for ever more precise theoretical templates of the binary dynamics and emit- ted waveform. The modeling of compact binary dynamics relies on"},{"citing_arxiv_id":"2604.13930","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Bayesian Analysis of Gravitational Wave Microlensing Effects from Galactic Double White Dwarfs","primary_cat":"astro-ph.GA","submitted_at":"2026-04-15T14:39:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian analysis of simulated Taiji observations shows microlensing from lenses above 10^5 solar masses can be distinguished from unlensed DWD signals when separation is below 3 Einstein radii, while lower masses or larger separations cannot.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Acernese, et al., Phys. Rev. Lett.116, 241103 (2016), arXiv:1606.04855 [gr-qc]. [27] B. P. Abbott, R. Abbott, T. D. Abbott, M. R. Abernathy, F. Acernese, et al., Phys. Rev. Lett.116, 221101 (2016), arXiv:1602.03841 [gr-qc]. [28] B. P. Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, et al., Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [29] B. P. Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, et al., Phys. Rev. Lett.121, 161101 (2018), arXiv:1805.11581 [gr-qc]. [30] R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, et al., Physical Re- view X13, 041039 (2023), arXiv:2111.03606 [gr-qc]. [31] B. P. Abbott, R. Abbott, T. D. Abbott, S. Abraham, F. Acernese, et al., Astrophys."},{"citing_arxiv_id":"2604.13208","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"NICER observations constrain the NS mass-radius relation, and thereby the underlying nu- clear equation of state, by measuring X-ray pulse pro- files from rotating NSs [2-5, 7, 8]. GW measurements of thetidaldeformabilityprovideimportantcomplementary constraints [12, 15]. Looking ahead, third-generation GW detectors such as the Einstein Telescope [16, 17] and Cosmic Explorer [18] are expected to resolve the oscilla- tion spectrum of NSs by accessing the post-merger GW emission of binary NS coalescences, opening yet another channel to probe matter under extreme conditions. These increasingly precise measurements must be matched by equally accurate theoretical models. To date, most studies do not consider in detail out-of-equilibrium"},{"citing_arxiv_id":"2604.13011","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"stability threshold beyond which no internal pressure can prevent gravitational collapse. In the modern era, the state 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"},{"citing_arxiv_id":"2604.11046","ref_index":88,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"model-independent, we define RX1.4(ρtr) = maxX 1.4 −minX 1.4 σX1.4 ,(5) where the numerator is the maximum spread across low-density EoS models at 1.4M ⊙ andσ X1.4 is the current 68% CI observational uncertainty. ForR 1.4 we compute the average error,σ R1.4 = 0.8 km fromR 1.4 = 11.36+0.95 −0.63 km [27], and for Λ 1.4 we convert the 90% CI result Λ 1.4 = 190 +390 −120 [88] to a 68% CI, yielding σΛ1.4 ≈200 1. We definepractical model independence asR X1.4 <1, i.e., the spread across models falls below current observational uncertainty. WhenR>1, model dependence is resolvable by current observations and must be accounted for in inference analyses. From Table II, atρ tr = 2ρ 0, bothR R1.4 = 1.79 andR Λ1.4 = 1.37 exceed unity, indicating significant"},{"citing_arxiv_id":"2604.04560","ref_index":84,"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":"Mishra, P. K. Panda, and W. Greiner,Vacuum polarization effects in hyperon rich dense matter: A Nonperturbative treatment,J. Phys. G28(2002) 67-83, [nucl-th/0101006]. [83] L. Tolos, M. Centelles, and A. Ramos,Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints,Astrophys. J.834(2017), no. 1 3, [arXiv:1610.00919]. [84] J. D. Walecka,Electromagnetic and Weak Interactions with Nuclei, in6th Symposium on Photoelectronic Image Devices, 9, 1974. [85] J. Boguta and A. R. Bodmer,Relativistic Calculation of Nuclear Matter and the Nuclear Surface,Nucl. Phys. A292(1977) 413-428. [86] J. Boguta and S. A. Moszkowski,NONLINEAR MEAN FIELD THEORY FOR NUCLEAR MATTER AND SURFACE PROPERTIES,Nucl."},{"citing_arxiv_id":"2601.18835","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Beyond FINDCHIRP: Breaking the memory wall and optimal FFTs for Gravitational-Wave Matched-Filter Searches with Ratio-Filter Dechirping","primary_cat":"astro-ph.IM","submitted_at":"2026-01-25T20:45:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Ratio-Filter Dechirping converts gravitational-wave matched filtering from a memory-bound FFT into a cache-efficient FIR convolution, delivering a measured 8x speedup in the core loop.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.24194","ref_index":9,"ref_count":1,"confidence":0.98,"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":"2512.19907","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Astrophysical constraints on the cold equation of state of the strongly interacting matter","primary_cat":"astro-ph.HE","submitted_at":"2025-12-22T22:21:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.05767","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tidal Love numbers for regular black holes","primary_cat":"gr-qc","submitted_at":"2025-12-05T14:54:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Tidal Love numbers of regular black holes are generically nonzero, model-dependent, and can acquire logarithmic scale dependence at higher perturbative orders.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.19626","ref_index":6,"ref_count":1,"confidence":0.98,"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":"2511.07226","ref_index":56,"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":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":"2510.22137","ref_index":11,"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":"2510.05400","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Binary Neutron Stars from the Moon: Early Warnings and Precision Science for the Artemis Era","primary_cat":"gr-qc","submitted_at":"2025-10-06T21:46:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Lunar GW observatories can deliver weeks-to-months early warnings, 0.01 deg² localizations, and ~100 well-localized BNS events per year for GW170817-like sources, with multi-band networks yielding 0.1% mass-ratio and 1% distance precision.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.06145","ref_index":3,"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":"2508.15912","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"$f$-mode Oscillations for Hyperons and H-dibaryons in Neutron Stars","primary_cat":"astro-ph.HE","submitted_at":"2025-08-21T18:18:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The study examines the effects of hyperons and H-dibaryons on f-mode oscillations in neutron stars using the quark meson coupling model and tests universal relations in the Cowling approximation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.16929","ref_index":79,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Properties of the neutron star crust informed by nuclear structure data","primary_cat":"nucl-th","submitted_at":"2025-05-22T17:22:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bayesian NS EoS study using full nuclear posterior distributions and consistent crust modeling finds increased surface thickness and crustal moment of inertia relative to prior work.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2502.01093","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A practical Bayesian method for gravitational-wave ringdown analysis with multiple modes","primary_cat":"gr-qc","submitted_at":"2025-02-03T06:31:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"FIREFLY accelerates multi-mode GW ringdown analysis by analytically marginalizing QNM amplitudes and phases via Bayesian principles and importance sampling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2010.14527","ref_index":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","primary_cat":"gr-qc","submitted_at":"2020-10-27T18:01:31+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":7.0,"formal_verification":"none","one_line_summary":"LIGO and Virgo detected 39 compact binary coalescence events in O3a, including 13 new ones, with black hole binaries up to 150 solar masses and the first significantly asymmetric mass ratios.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"In addition to BBHs, Advanced LIGO and Advanced Virgo detected the first gravita- tional wave signal from a binary neutron star (BNS) coalescence, GW170817 [12], which was also the first joint detection of gravitational waves and electromag- netic emission [13, 14]. Gravitational wave discoveries have had a profound impact on physics, astronomy and astrophysics [13, 15-19], and the public release of LIGO and Virgo data [20, 21] has enabled groups other than the LIGO Scientific Collaboration and Virgo Collabo- ration (LVC) to perform analyses searching for gravita- tional wave signals [22-28] and to report additional can- didate events in some cases. We present the results of searches for compact binaries in Advanced LIGO and Advanced Virgo data taken be-"},{"citing_arxiv_id":"2006.00714","ref_index":203,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bayesian inference for compact binary coalescences with BILBY: Validation and application to the first LIGO--Virgo gravitational-wave transient catalogue","primary_cat":"astro-ph.IM","submitted_at":"2020-06-01T04:46:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"BILBY is validated on simulated compact binary signals and reproduces the eleven GWTC-1 results with configuration and output files provided for reproduction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1912.02622","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Science Case for the Einstein Telescope","primary_cat":"astro-ph.CO","submitted_at":"2019-12-05T14:57:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"The Einstein Telescope will enable gravitational-wave observations up to cosmological distances, opening avenues for discoveries in astrophysics, cosmology, and fundamental physics.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"With 2G detectors, the first observed NS-NS coalescence GW170817 demonstrated that use- ful limits on the NSs' tidal deformability, a characteristic parameter that depends on the properties of matter in their interiors, could be extracted from the inspiral part of the GW signal [2]. However, despite the proximity of GW170817, the inferred constraints on the equation of state of NS matter [37] are too weak to discriminate between realistic models, nor do they offer new insights about phase transitions [38-40]. To determine in detail the nature of matter and interactions in NS interiors requires measuring tidal deformability with an order of magnitude higher accuracy. In addition, such high-fidelity measurements must be obtained for a population of NSs spanning a wide"},{"citing_arxiv_id":"1907.06597","ref_index":88,"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":"1811.02042","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Bilby: A user-friendly Bayesian inference library for gravitational-wave astronomy","primary_cat":"astro-ph.IM","submitted_at":"2018-11-05T21:35:34+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bilby introduces a user-friendly Python library for accurate Bayesian inference on gravitational-wave signals from compact binaries and other sources, including hierarchical population modeling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"with straightforward syntax and tools that facilitate use arXiv:1811.02042v1 [astro-ph.IM] 5 Nov 2018 2 by beginners. For example, with minimal user effort, users can download and analyze publicly-available LIGO and Virgo data to obtain posterior distributions for the astrophysical parameters associated with recent detec- tions of binary black holes [3, 16, 23-26] and the binary neutron star merger [6]. One key functional difference between Bilby and LALInference/PyCBC Inference is its modular- ity and adaptability. The core library is not specific to gravitational-wave science and has uses outside of the gravitational-wave community. Ongoing projects in- clude astrophysical inference in multimessenger astron- omy, pulsar timing, and x-ray observations of accreting"}],"limit":50,"offset":0}