{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:QWZPXYL4FBRNZYOUHQTQG5VGUZ","short_pith_number":"pith:QWZPXYL4","schema_version":"1.0","canonical_sha256":"85b2fbe17c2862dce1d43c270376a6a6762a62b82384ebdbe1690c45142df5b6","source":{"kind":"arxiv","id":"2111.05350","version":2},"attestation_state":"computed","paper":{"title":"How perturbative QCD constrains the Equation of State at Neutron-Star densities","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"nucl-th","authors_text":"Aleksi Kurkela, Oleg Komoltsev","submitted_at":"2021-11-09T19:00:03Z","abstract_excerpt":"We demonstrate in a general and analytic way how high-density information about the equation of state (EoS) of strongly interacting matter obtained using perturbative Quantum Chromodynamics (pQCD) constrains the same EoS at densities reachable in physical neutron stars. Our approach is based on utilizing the full information of the thermodynamic potentials at the high-density limit together with thermodynamic stability and causality. This requires considering the pressure as a function of chemical potential $p(\\mu)$ instead of the commonly used pressure as a function of energy density $p(\\epsi"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2111.05350","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"nucl-th","submitted_at":"2021-11-09T19:00:03Z","cross_cats_sorted":["astro-ph.HE","hep-ph"],"title_canon_sha256":"90e3d7f6b3a7854b3e57c5826f78d6b1d8885ccbe8a1a18abf3c9b956fdbebc8","abstract_canon_sha256":"90350c4436e6449e2355a0215abb9743f267a48ae556100819070fa9b1f6704e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:24:23.527530Z","signature_b64":"q63LALV80UnBq6wfAf4Sj8xh6y5FvYGJLiv+Ho6Ik8VRW1VgjY3eFP/76xdlGt6dxT5PWkgsbwKjc2XE4rNsAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"85b2fbe17c2862dce1d43c270376a6a6762a62b82384ebdbe1690c45142df5b6","last_reissued_at":"2026-07-05T04:24:23.527055Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:24:23.527055Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"How perturbative QCD constrains the Equation of State at Neutron-Star densities","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"nucl-th","authors_text":"Aleksi Kurkela, Oleg Komoltsev","submitted_at":"2021-11-09T19:00:03Z","abstract_excerpt":"We demonstrate in a general and analytic way how high-density information about the equation of state (EoS) of strongly interacting matter obtained using perturbative Quantum Chromodynamics (pQCD) constrains the same EoS at densities reachable in physical neutron stars. Our approach is based on utilizing the full information of the thermodynamic potentials at the high-density limit together with thermodynamic stability and causality. This requires considering the pressure as a function of chemical potential $p(\\mu)$ instead of the commonly used pressure as a function of energy density $p(\\epsi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2111.05350","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2111.05350/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"2111.05350","created_at":"2026-07-05T04:24:23.527105+00:00"},{"alias_kind":"arxiv_version","alias_value":"2111.05350v2","created_at":"2026-07-05T04:24:23.527105+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2111.05350","created_at":"2026-07-05T04:24:23.527105+00:00"},{"alias_kind":"pith_short_12","alias_value":"QWZPXYL4FBRN","created_at":"2026-07-05T04:24:23.527105+00:00"},{"alias_kind":"pith_short_16","alias_value":"QWZPXYL4FBRNZYOU","created_at":"2026-07-05T04:24:23.527105+00:00"},{"alias_kind":"pith_short_8","alias_value":"QWZPXYL4","created_at":"2026-07-05T04:24:23.527105+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":11,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.25186","citing_title":"Causality alone bounds the maximum radius difference between different-mass neutron stars","ref_index":25,"is_internal_anchor":false},{"citing_arxiv_id":"2606.21617","citing_title":"Hyperonic equation of state for neutron stars: A systematic Bayesian comparison of density-dependent and non-linear relativistic mean-field models","ref_index":38,"is_internal_anchor":false},{"citing_arxiv_id":"2606.21435","citing_title":"Is the coexistence of strange quark stars and hadronic stars favored by astrophysical data? A Bayesian analysis","ref_index":6,"is_internal_anchor":false},{"citing_arxiv_id":"2606.02966","citing_title":"Sensitivity of the Neutron Star Equation of State Inferences to Mass and Radius Measurements","ref_index":31,"is_internal_anchor":false},{"citing_arxiv_id":"2605.30369","citing_title":"Reconciling GW170817 and GW190814 with a Nonmonotonic Sound-Speed Equation of State","ref_index":36,"is_internal_anchor":false},{"citing_arxiv_id":"2605.08584","citing_title":"The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover","ref_index":19,"is_internal_anchor":false},{"citing_arxiv_id":"2606.29576","citing_title":"Quark and hybrid stars with renormalization group improvement of NNLO perturbative QCD","ref_index":38,"is_internal_anchor":false},{"citing_arxiv_id":"2509.06145","citing_title":"Equation of State Extrapolation Systematics: Parametric vs. Nonparametric Inference of Neutron Star Structure","ref_index":22,"is_internal_anchor":false},{"citing_arxiv_id":"2601.07931","citing_title":"General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly","ref_index":5,"is_internal_anchor":false},{"citing_arxiv_id":"2605.08584","citing_title":"The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover","ref_index":23,"is_internal_anchor":false},{"citing_arxiv_id":"2604.24949","citing_title":"A Physics Informed Bayesian Neural Network for the Neutron Star Equation of State","ref_index":48,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ","json":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ.json","graph_json":"https://pith.science/api/pith-number/QWZPXYL4FBRNZYOUHQTQG5VGUZ/graph.json","events_json":"https://pith.science/api/pith-number/QWZPXYL4FBRNZYOUHQTQG5VGUZ/events.json","paper":"https://pith.science/paper/QWZPXYL4"},"agent_actions":{"view_html":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ","download_json":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ.json","view_paper":"https://pith.science/paper/QWZPXYL4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2111.05350&json=true","fetch_graph":"https://pith.science/api/pith-number/QWZPXYL4FBRNZYOUHQTQG5VGUZ/graph.json","fetch_events":"https://pith.science/api/pith-number/QWZPXYL4FBRNZYOUHQTQG5VGUZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ/action/storage_attestation","attest_author":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ/action/author_attestation","sign_citation":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ/action/citation_signature","submit_replication":"https://pith.science/pith/QWZPXYL4FBRNZYOUHQTQG5VGUZ/action/replication_record"}},"created_at":"2026-07-05T04:24:23.527105+00:00","updated_at":"2026-07-05T04:24:23.527105+00:00"}