{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:FECGLVVHLDD3AJ6J4DXOES4J2O","short_pith_number":"pith:FECGLVVH","schema_version":"1.0","canonical_sha256":"290465d6a758c7b027c9e0eee24b89d3a18640508eec4e3339b18a23629933c0","source":{"kind":"arxiv","id":"2204.14039","version":3},"attestation_state":"computed","paper":{"title":"Perturbative QCD and the Neutron Star Equation of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"nucl-th","authors_text":"Ingo Tews, J\\'er\\^ome Margueron, Rahul Somasundaram","submitted_at":"2022-04-29T12:25:33Z","abstract_excerpt":"We construct a physics-agnostic approach to the neutron star (NS) equation of state (EoS) based on a sound speed model, which connects both low-density information from nuclear theory and high-density constraints from perturbative QCD (pQCD). Using this approach, we study the impact of pQCD calculations on NS EoS that have been constrained by astrophysical observations. We find that pQCD affects the EoS mainly beyond the densities realized in NS. Furthermore, we observe an interesting interplay between pQCD and astrophysical constraints, with pQCD preferring softer EoS for the heaviest NS whil"},"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":"2204.14039","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2022-04-29T12:25:33Z","cross_cats_sorted":[],"title_canon_sha256":"0ba147791112ae926cede39fd42483e067c9dadcbf7eb9db82bbdbf7fdb92019","abstract_canon_sha256":"cee1cb56672345eb4d4a26079f1960e76d7abab394657618dc919d63cab03291"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:42:39.353370Z","signature_b64":"byV7HHBg6vN1FZl7CQGR7JO6M3+UY31lQaJWU5wACm/bJ4GIT6EPnQbi2r8TrPcJps/vDxoujgsBkPomT9KODw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"290465d6a758c7b027c9e0eee24b89d3a18640508eec4e3339b18a23629933c0","last_reissued_at":"2026-07-05T06:42:39.352868Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:42:39.352868Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Perturbative QCD and the Neutron Star Equation of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"nucl-th","authors_text":"Ingo Tews, J\\'er\\^ome Margueron, Rahul Somasundaram","submitted_at":"2022-04-29T12:25:33Z","abstract_excerpt":"We construct a physics-agnostic approach to the neutron star (NS) equation of state (EoS) based on a sound speed model, which connects both low-density information from nuclear theory and high-density constraints from perturbative QCD (pQCD). Using this approach, we study the impact of pQCD calculations on NS EoS that have been constrained by astrophysical observations. We find that pQCD affects the EoS mainly beyond the densities realized in NS. Furthermore, we observe an interesting interplay between pQCD and astrophysical constraints, with pQCD preferring softer EoS for the heaviest NS whil"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2204.14039","kind":"arxiv","version":3},"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/2204.14039/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":"2204.14039","created_at":"2026-07-05T06:42:39.352926+00:00"},{"alias_kind":"arxiv_version","alias_value":"2204.14039v3","created_at":"2026-07-05T06:42:39.352926+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2204.14039","created_at":"2026-07-05T06:42:39.352926+00:00"},{"alias_kind":"pith_short_12","alias_value":"FECGLVVHLDD3","created_at":"2026-07-05T06:42:39.352926+00:00"},{"alias_kind":"pith_short_16","alias_value":"FECGLVVHLDD3AJ6J","created_at":"2026-07-05T06:42:39.352926+00:00"},{"alias_kind":"pith_short_8","alias_value":"FECGLVVH","created_at":"2026-07-05T06:42:39.352926+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.08584","citing_title":"The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover","ref_index":34,"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":7,"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":28,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O","json":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O.json","graph_json":"https://pith.science/api/pith-number/FECGLVVHLDD3AJ6J4DXOES4J2O/graph.json","events_json":"https://pith.science/api/pith-number/FECGLVVHLDD3AJ6J4DXOES4J2O/events.json","paper":"https://pith.science/paper/FECGLVVH"},"agent_actions":{"view_html":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O","download_json":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O.json","view_paper":"https://pith.science/paper/FECGLVVH","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2204.14039&json=true","fetch_graph":"https://pith.science/api/pith-number/FECGLVVHLDD3AJ6J4DXOES4J2O/graph.json","fetch_events":"https://pith.science/api/pith-number/FECGLVVHLDD3AJ6J4DXOES4J2O/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O/action/storage_attestation","attest_author":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O/action/author_attestation","sign_citation":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O/action/citation_signature","submit_replication":"https://pith.science/pith/FECGLVVHLDD3AJ6J4DXOES4J2O/action/replication_record"}},"created_at":"2026-07-05T06:42:39.352926+00:00","updated_at":"2026-07-05T06:42:39.352926+00:00"}