{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:K62Z352OWC7DHXCGYKCI6GH5CR","short_pith_number":"pith:K62Z352O","schema_version":"1.0","canonical_sha256":"57b59df74eb0be33dc46c2848f18fd1450e0be8e1841a19306aa1ffeeacf7b40","source":{"kind":"arxiv","id":"2312.10148","version":2},"attestation_state":"computed","paper":{"title":"Which first order phase transitions to quark matter are possible in neutron stars?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"nucl-th","authors_text":"Jan-Erik Christian, J\\\"urgen Schaffner-Bielich, Stephan Rosswog","submitted_at":"2023-12-15T19:00:26Z","abstract_excerpt":"We examine which first order phase transitions are consistent with today's astrophysical constraints. In particular, we explore how a well-constrained mass-radius data point would restrict the admissible parameter space and to this end, we employ the most likely candidates of the recent NICER limits of PSR J0030+0451. To systematically vary the stiffness of the equation of state, we employ a parameterizable relativistic mean field equation of state, which is in compliance with results from chiral effective field theory. We model phase transitions via Maxwell constructions and parameterize them"},"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":"2312.10148","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2023-12-15T19:00:26Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"6a351994cd2c5aae58259486e4bb24ebcbc90d644467759dc4c1dd362895759b","abstract_canon_sha256":"5e704a7e3efbcf513929b65520fa6ef3eadf176584741c4013e25fce09cabdf0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:59:59.020158Z","signature_b64":"PfgWtwwye5xlF1et4GM5GXgET4JfjUXQBbWExYEVDnUn8h3xIOCbJXTXT7ntnC8HviFeeh0siRzNkMGUvhCcAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"57b59df74eb0be33dc46c2848f18fd1450e0be8e1841a19306aa1ffeeacf7b40","last_reissued_at":"2026-07-05T07:59:59.019676Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:59:59.019676Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Which first order phase transitions to quark matter are possible in neutron stars?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"nucl-th","authors_text":"Jan-Erik Christian, J\\\"urgen Schaffner-Bielich, Stephan Rosswog","submitted_at":"2023-12-15T19:00:26Z","abstract_excerpt":"We examine which first order phase transitions are consistent with today's astrophysical constraints. In particular, we explore how a well-constrained mass-radius data point would restrict the admissible parameter space and to this end, we employ the most likely candidates of the recent NICER limits of PSR J0030+0451. To systematically vary the stiffness of the equation of state, we employ a parameterizable relativistic mean field equation of state, which is in compliance with results from chiral effective field theory. We model phase transitions via Maxwell constructions and parameterize them"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2312.10148","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/2312.10148/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":"2312.10148","created_at":"2026-07-05T07:59:59.019738+00:00"},{"alias_kind":"arxiv_version","alias_value":"2312.10148v2","created_at":"2026-07-05T07:59:59.019738+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2312.10148","created_at":"2026-07-05T07:59:59.019738+00:00"},{"alias_kind":"pith_short_12","alias_value":"K62Z352OWC7D","created_at":"2026-07-05T07:59:59.019738+00:00"},{"alias_kind":"pith_short_16","alias_value":"K62Z352OWC7DHXCG","created_at":"2026-07-05T07:59:59.019738+00:00"},{"alias_kind":"pith_short_8","alias_value":"K62Z352O","created_at":"2026-07-05T07:59:59.019738+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.17875","citing_title":"Hybrid Stars with Post-Merger Rotation Profiles","ref_index":32,"is_internal_anchor":false},{"citing_arxiv_id":"2503.19691","citing_title":"Strongly Interacting Dark Matter admixed Neutron Stars","ref_index":79,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR","json":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR.json","graph_json":"https://pith.science/api/pith-number/K62Z352OWC7DHXCGYKCI6GH5CR/graph.json","events_json":"https://pith.science/api/pith-number/K62Z352OWC7DHXCGYKCI6GH5CR/events.json","paper":"https://pith.science/paper/K62Z352O"},"agent_actions":{"view_html":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR","download_json":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR.json","view_paper":"https://pith.science/paper/K62Z352O","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2312.10148&json=true","fetch_graph":"https://pith.science/api/pith-number/K62Z352OWC7DHXCGYKCI6GH5CR/graph.json","fetch_events":"https://pith.science/api/pith-number/K62Z352OWC7DHXCGYKCI6GH5CR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR/action/storage_attestation","attest_author":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR/action/author_attestation","sign_citation":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR/action/citation_signature","submit_replication":"https://pith.science/pith/K62Z352OWC7DHXCGYKCI6GH5CR/action/replication_record"}},"created_at":"2026-07-05T07:59:59.019738+00:00","updated_at":"2026-07-05T07:59:59.019738+00:00"}