{"total":16,"items":[{"citing_arxiv_id":"2606.09247","ref_index":20,"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":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"the shear properties are carried out in this hypothesis. The shear speed can be also used to evaluate the fre- quency of the fundamental (n= 0) torsional oscillation crust mode, denoted as lt0. The latter can be estimated through a plane-wave analysis of the crustal (axial) pertur- bation equations as (Piro 2005; Samuelsson & Andersson 2007) ω0 ≈ e2νv2 s(l−1)(l+ 2) 2RRcc ,(20) wheree 2ν = 1−2GM/(Rc 2), withMandRthe NS mass and radius, respectively,Gthe gravitational constant, and Rcc the radius at the crust-core transition. As discussed in Samuelsson & Andersson (2007), the approximation in Eq. (20) is based on the assumptionω0 ≫e 2νv2 s(l−1)(l+ 2)/r2, that is not necessarily satisfied throughout the crust. Moreover, to computeω 0, one can either assume an aver-"},{"citing_arxiv_id":"2605.28944","ref_index":110,"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":"2605.26228","ref_index":116,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Donutization Inside Neutron Stars: Shell-Localized Scalar Fields","primary_cat":"gr-qc","submitted_at":"2026-05-25T18:00:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Heavy scalar fields in neutron stars form interior shell-localized profiles that reshape the effective equation of state and break the I-Q relation while remaining hidden from binary pulsar observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19731","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neutron stars more compact than black holes in quasi-topological gravity: Equilibrium configurations and radial stability","primary_cat":"gr-qc","submitted_at":"2026-05-19T12:05:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In quasi-topological gravity, neutron stars can surpass black-hole compactness with universal high-density behavior and theory corrections that stabilize radially unstable configurations from general relativity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10467","ref_index":43,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Axial Quasi-normal Modes of Admixed Neutron Stars","primary_cat":"hep-ph","submitted_at":"2026-05-11T12:33:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Increasing the bosonic dark matter fraction in admixed neutron stars shifts axial quasi-normal mode frequencies and damping times, can reorder mode hierarchy, and drives a transition from neutron-star-like to boson-star-like ringdown behavior.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"with dark-matter cores may help distinguish such systems from ordinary NS mergers. Related studies have also explored a variety of properties of hybrid admixed compact stars [37-42]. The advent of gravitational-wave astronomy has turned compact-object mergers into a powerful probe of the dark sector. The detections of binary black-hole mergers by LIGO and Virgo [43], as well as the multimessenger event GW170817 from a binary NS merger [44], have shown that gravitational-wave signals carry direct information about the internal structure and equation of state of compact objects. In systems containing a BS, or in BS-NS or BS-black hole mergers, the gravitational-wave signal may exhibit a distinctive late-time ringdown that reflects the nature of the underlying dark matter and its self-interactions."},{"citing_arxiv_id":"2605.01737","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Axial $w$-modes of anisotropic neutron stars","primary_cat":"gr-qc","submitted_at":"2026-05-03T06:25:47+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":"Chamel, J. M. Pear- son, and S. Goriely, Analytical representations of unified equations of state for neutron-star matter, Astron. Astro- phys.560, A48 (2013), arXiv:1310.0049 [astro-ph.SR]. [54] F. Douchin and P. Haensel, A unified equation of state of dense matter and neutron star structure, Astron. As- trophys.380, 151 (2001), arXiv:astro-ph/0111092. [55] E. Chabanat, P. Bonche, P. Haensel, J. Meyer, and R. Schaeffer, A Skyrme parametrization from subnuclear to neutron star densities Part II. Nuclei far from stabili- ties, Nucl. Phys. A635, 231 (1998). [56] D. Horvat, S. Ilijic, and A. Marunovic, Radial pulsations and stability of anisotropic stars with quasi-local equa- tion of state, Class. Quant."},{"citing_arxiv_id":"2605.01436","ref_index":76,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on Einstein-aether gravity from the precision timing of PSR J1738+0333","primary_cat":"gr-qc","submitted_at":"2026-05-02T13:19:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Precision timing of PSR J1738+0333 from EPTA and NANOGrav data yields the tightest strong-field constraints on Einstein-aether parameters from any single binary pulsar.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"ble impact on our results; we therefore adopt theAPR EoS [41] for definiteness. To quantify the residual EoS dependence, we compute the relative difference in the predicted ˙Pb with respect to the APR value, using our best estimates ofm p,m c,P b, ande, across the full pa- rameter space ofα 1,α 2, andc ω within their prior ranges. For softer EoS models, such as WFF1 [75] and SLY4 [76], this difference remains below 1.5% throughout. 1.50 1.25 1.00 0.75 0.50 0.25 0.00 1 ×10 4 7.2 × 10 5 4.4 × 10 5 Posterior p( 1) P( 1 > x) = 90% P( 1 > x) = 68% FIG. 3. Posterior probability density ofα 1 for PSR J1738+0333. The shaded regions and dashed vertical lines mark the one-sided lower bounds at 68% (orange) and 90% (red) credible level."},{"citing_arxiv_id":"2604.24949","ref_index":37,"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":"method","top_context_polarity":"use_method","context_text":"in the near-saturation regime and typically require additional high-density priors (e.g., causality and pQCD matching) for inner-core extrapolation. d. Bayesian Power Regression model with heteroscedastic errors (BPR-HE):In Ref. [33], we 3 introduced BPR-HE as a Bayesian alternative to segmented piecewise polytrope fits, trained on 65 hadronic EoSs from the LIGO LALSuite infrastructure [37]. The model uses a continuous power-law mean relation, P(ϵ) =a ϵ b,(2) whereasets the pressure scale andbcontrols effective stiffness. In log-space, the regression is linear, and BPR-HE captures density-dependent spread with a heteroscedastic likelihood,y i ∼ N(α+blnϵ i, σ2(ϵi)), usingσ(ϵ) =s m(ϵ/ϵref)m. This yields positive (log- normal) pressure predictions and propagates uncertainty"},{"citing_arxiv_id":"2604.08651","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Primordial Neutron Stars","primary_cat":"astro-ph.CO","submitted_at":"2026-04-09T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Large initial baryon asymmetry allows Hubble patches to collapse into primordial neutron stars arrested by nuclear pressure, requiring later entropy dilution to match observed Y_B and BBN.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"number ofe-folds during EDE. After reheating, a relativistic bath of SM particles is created with reheat temperature that satisfiesT RH < ΛQCD to ensure that baryons inside the PNS are not con- verted into relativistic quarks, which would destroy any PNS formed during baryon domination; we also demand thatT RH ≳MeV to allow for standard BBN to proceed [29]. If no net baryons are created during reheating, the baryon-to-entropy ratio satisfies YB(aRH) = nB(aRH) s(aRH) = 3TRH 2mp e−3Ne ,(11) wheres(a RH) is the entropy density at reheating and we have neglected residual radiation in the last step, which is valid for largeY B(aBG) - see Appendix C for a discussion. In Fig. 2 we show the parameter space that realizes the"},{"citing_arxiv_id":"2512.24194","ref_index":47,"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":"2511.06489","ref_index":34,"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":"2510.11861","ref_index":32,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of facility timing and coordination for next-generation gravitational-wave detectors","primary_cat":"gr-qc","submitted_at":"2025-10-13T19:15:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations of ET and CE networks show delays degrade localization metrics far more than SNR, with LIGO India greatly reducing the impact for multi-messenger and stochastic searches.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.06145","ref_index":35,"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":"2507.15951","ref_index":132,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves $-$ Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter","primary_cat":"hep-ph","submitted_at":"2025-07-21T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Future high-frequency-sensitive GW detectors can distinguish binary neutron star from low-mass black hole mergers in late phases, enabling separation of merger rates and constraints on heavy non-annihilating dark matter via transmuted black holes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"quantities are calculated, with values 450 M⊙, 600M⊙, 800M⊙, and 1000 M⊙. −0.02 −0.01 0.00 0.01 0.02 Time t [sec] 10−23 10−22 10−21 10−20 Strain h(t) EoS SLy, DL = 1 Mpc 500 1000 1500 2000 2500 3000 3500 4000 Frequency f [Hz] 10−25 10−24 10−23 10−22 Strain ˜h(f ) [sec] EoS SLy, DL = 1 Mpc Figure 10: The time domain and frequency domain strain amplitudes are shown for the SLy EoS [132, 133], obtained from the BAM:0098 waveform dataset. Waveforms corresponding to seven additional EoSs have been extracted using the same procedure. For subsequent analysis, the frequency domain representations are used. Strain vs Frequency Waveform from BAM:0098 As an example, consider BAM:0098.h5 which is simulated with the EoS SLy [132, 133], with initial parameters as per our requirement."},{"citing_arxiv_id":"2505.16929","ref_index":38,"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":"2312.01406","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neutron stars more compact than black holes as a probe of strong-field gravity","primary_cat":"gr-qc","submitted_at":"2023-12-03T14:09:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Stable neutron-star configurations denser than black holes exist in quasi-topological gravity and may produce detectable gravitational-wave echoes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}