{"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","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Bayesian inference shows that the mass and density-profile parameter of sub-GeV dark matter in neutron stars are nearly independent of the hadronic model for moderate symmetry-energy slopes.","cross_cats":["hep-ph","hep-th"],"primary_cat":"nucl-th","authors_text":"Atanu Guha, Chang Ho Hyun, Debashree Sen","submitted_at":"2026-05-14T06:41:34Z","abstract_excerpt":"We study the impact of symmetry energy ($S$), hyperons, and dark matter (DM) on structural and oscillatory properties of neutron stars (NSs). Uncertainty from hadronic equation of state for NSs is considered with 15 relativistic mean field models having slope parameter ($L_0$) of $S$ in range $40-120$ MeV. DM admixed NSs (DMANSs) are described with feeble interaction between light DM fermions ($\\chi$) with hadronic matter in the presence of hyperons via scalar ($\\eta$) and vector ($\\xi$) dark mediators. The masses $m_{\\chi}$, $m_{\\eta}$ and $m_{\\xi}$ are related by self-interaction constraints"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"Employing models of DMANSs that satisfy several observational data, we infer with Bayesian analysis, the likely ranges of m_χ and α are almost independent of the underlying hadronic model within 40 MeV ≲ L0 < 58 MeV.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The assumption that the dark-matter density profile inside the star can be written as an exponential function of baryon density controlled by a single free parameter α, together with the requirement that dark matter contributes less than 10 percent to the total mass.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"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,","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Bayesian inference shows that the mass and density-profile parameter of sub-GeV dark matter in neutron stars are nearly independent of the hadronic model for moderate symmetry-energy slopes.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"f787dc69b7becc669be5c1783e5d6deb95c6f92622abca93e5a393faf19f366c"},"source":{"id":"2605.14447","kind":"arxiv","version":1},"verdict":{"id":"9dd51fab-3992-4d9f-9f15-06d45f09eb27","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-15T01:42:53.572215Z","strongest_claim":"Employing models of DMANSs that satisfy several observational data, we infer with Bayesian analysis, the likely ranges of m_χ and α are almost independent of the underlying hadronic model within 40 MeV ≲ L0 < 58 MeV.","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,","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The assumption that the dark-matter density profile inside the star can be written as an exponential function of baryon density controlled by a single free parameter α, together with the requirement that dark matter contributes less than 10 percent to the total mass.","pith_extraction_headline":"Bayesian inference shows that the mass and density-profile parameter of sub-GeV dark matter in neutron stars are nearly independent of the hadronic model for moderate symmetry-energy slopes."},"references":{"count":140,"sample":[{"doi":"","year":1940,"title":"Heavy-mass stars are relevant to the effect of exotic degrees of freedom like hyperons and quark matter","work_id":"5f1cafcf-a159-482f-944c-08538e9ee068","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"= X B=N,Y gωB ρB,(20) m2 ρρ03 + 2Λωρ(g2 ωN ω2 0)(g2 ρN ρ03) = X B=N,Y gρB 2 τ3BρB,(21) and m2 ϕϕ0 +d 3ϕ3 0 + 2Λϕρ(g2 ϕN ϕ2 0)(g2 ρN ρ2","work_id":"c1531616-1801-4664-bada-a6682b87c7d7","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"(11) and (18), respectively, except for the fact that the couplings are density independent and Σ R=0 in Eq","work_id":"45833b02-58be-44c4-93a4-0ee6f43cfa2e","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"The permitted values ofm η andm ξ corresponding to the range ofm χ are already shown in our previous works [37, 38, 48]","work_id":"f4dda697-c34b-42cb-9443-7c20486f9fd4","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":null,"title":"and corresponding radius [25] are also indicated. The constraints onM−Rplane prescribed from GW170817 [21], the NICER experiment for PSR J0030+0451 [22], HESS J1731-347 [26], PSR J0437-4715 [23], and ","work_id":"2d64b62d-ad71-4aa3-a413-350c739e47e9","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":140,"snapshot_sha256":"b1c5726c30d4579d49d3a9b9bbcb8ff52389c09dc6a7e2004adf355065b0dd61","internal_anchors":34},"formal_canon":{"evidence_count":2,"snapshot_sha256":"29aefa930d2e79fa60e374b360cd0b61f3015f2a85c6cd1f12a6a48327940815"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}