{"total":10,"items":[{"citing_arxiv_id":"2605.14447","ref_index":40,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"Rafiei Karkevandi, JCAP03, 017 (2026), 2510.08115. [36] A. Del Popolo, M. Deliyergiyev, and M. Le Delliou, Phys. Dark Univ.30, 100622 (2020), 2011.00984. [37] D. Sen and A. Guha, Mon. Not. Roy. Astron. Soc.504, 3354 (2021), 2104.06141. [38] A. Guha and D. Sen, JCAP09, 027 (2021), 2106.10353. [39] A. Guha and D. Sen, Phys. Rev. D109, 043038 (2024), 2401.14419. [40] S. W. Randall, M. Markevitch, D. Clowe, A. H. Gonzalez, and M. Bradac, Astrophys. J.679, 1173 (2008), 0704.0261. [41] M. Bradac, D. Clowe, A. H. Gonzalez, P. Marshall, W. Forman, C. Jones, M. Markevitch, S. Randall, T. Schrabback, and D. Zaritsky, Astrophys. J.652, 937 (2006), astro-ph/0608408. [42] S. Tulin, H.-B. Yu, and K. M. Zurek, Phys. Rev. D87, 115007 (2013), 1302."},{"citing_arxiv_id":"2605.09206","ref_index":7,"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":"05702. [6] M. C. Miller, F. K. Lamb, A. J. Dittmann, S. Bogdanov, Z. Arzoumanian, K. C. Gendreau, S. Guillot, A. K. Harding, W. C. G. Ho, J. M. Lattimer, R. M. Ludlam, S. Mahmoodifar, S. M. Morsink, P. S. Ray, T. E. Strohmayer, K. S. Wood, T. Enoto, R. Foster, T. Okajima, G. Prigozhin, and Y. Soong, The Astrophysical Journal887, L24 (2019), 1912.05705. [7] T. E. Riley, A. L. Watts, P. S. Ray, S. Bogdanov, S. Guillot, S. M. Morsink, A. V. Bilous, Z. Arzoumanian, D. Choudhury, J. S. Deneva, K. C. Gendreau, A. K. Harding, W. C. G. Ho, J. M. Lattimer, M. Loewenstein, R. M. Ludlam, C. B. Markwardt, T. Okajima, C. Prescod-Weinstein, R. A. Remillard, M. T. Wolff, E. Fonseca, H. T. Cromartie, M. Kerr, T. T."},{"citing_arxiv_id":"2605.05005","ref_index":13,"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":"method","top_context_polarity":"use_method","context_text":"We employ the RMF model with the BigApple param- eterization [43] to describe the hadronic matter, where nucleons interact through the exchange of various mesons including the isoscalar-scalarσmeson, the isoscalar- vectorωmeson, and the isovector-vectorρmeson. The Lagrangian density for hadronic matter consisting of nu- cleons (pandn) and leptons (e) is written as [13, 20, 31- 33] L= ¯ψ(iγµ∂µ −m N)ψ+ 1 2(∂µσ∂ µσ−m 2 σσ2)− 1 4 ωµν ωµν + 1 2 m2 ωωµωµ − 1 4 ρµν ρµν + 1 2 m2 ρ ⃗ ρµ ⃗ρµ + (gσ ¯ψσψ−g ω ¯ψγµωµψ− 1 2 gρ ¯ψγµ⃗ τ .⃗ρµ)− 1 3 bm(gσσ)3 − c 4(gσσ)4 + Λωg2 ω(ωµωµ)(g2 ρ⃗ ρµ ⃗ρµ) + ζ 4!(g2 ωωµωµ)2 + X l=e ¯ψl(iγµ∂µ −m l)ψl .(1) The mean field equations are : m2 σ σ0 =−m b g 3 σσ2 0 −cg 4 σσ3 0 +g σ(ρs p +ρ s n),"},{"citing_arxiv_id":"2604.24949","ref_index":20,"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":", Physical Review D111, 083056 (2025), 2501.18544. [17] I. Liodis, E. Smyrniotis, and N. Stergioulas, Physical Review D109, 104008 (2024), 2309.03991. [18] Y. Fujimotoet al., Physical Review D110, 034035 (2024), 2401.12688. [19] N. Stergioulas, inCompact Objects in the Universe, edited by E. Papantonopoulos and N. Mavromatos (Cham, 2024) pp. 329-356. [20] S. Nget al., Classical and Quantum Gravity42, 205008 (2025), 2507.03232. [21] J.-J. Li, Y. Tian, and A. Sedrakian, Physical Review C 111, 055804 (2025), 2502.20000. [22] X. Donget al., Physical Review D112, 063043 (2025), 2509.03069. [23] J.-J. Li and A. Sedrakian, Physical Review C112, 015802 (2025), 2505.00911. [24] J.-J. Li, Y. Tian, and A. Sedrakian, Physics Letters B"},{"citing_arxiv_id":"2604.02782","ref_index":14,"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":"lay method-based on the extra time radio pulses take to traverse the gravitational field of a companion-has been key in measuring the masses of massive pulsars in a binary with a white dwarf [10]. The first such measurement, for PSR J1614-2230, yielded a mass of 1.908(16)M ⊙ [11-13]. The second, PSR J0348+0432, was found to haveM= 2.01±0.04M ⊙ using combined timing and optical modeling [14]. The most massive to date known neutron star, PSR J0740+6620, has a mea- sured mass of 2.08±0.07M ⊙ [15]. In general relativity, stability requires that stellar mass increase with central density according to the Bardeen- Thorne-Meltzer criterion [16], which is equivalent to the requirement that the oscillation modes of the star re- main stable on acsending branch of mass-central density"},{"citing_arxiv_id":"2601.07931","ref_index":36,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2508.15912","ref_index":31,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2105.06979","ref_index":43,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Radius of PSR J0740+6620 from NICER and XMM-Newton Data","primary_cat":"astro-ph.HE","submitted_at":"2021-05-14T17:33:32+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"PSR J0740+6620 has an equatorial radius of 13.7^{+2.6}_{-1.5} km, and multi-messenger data constrain 1.4 and 2.08 solar-mass neutron star radii to 12.45 and 12.35 km respectively.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}