{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:XXMV7NX2FHT7KAIXD3O2Y6XP45","short_pith_number":"pith:XXMV7NX2","schema_version":"1.0","canonical_sha256":"bdd95fb6fa29e7f501171eddac7aefe75b20c53d326f70ed681d35f192111466","source":{"kind":"arxiv","id":"2205.03455","version":1},"attestation_state":"computed","paper":{"title":"A new class of hybrid EoS with multiple critical endpoints for simulations of supernovae, neutron stars and their mergers","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"nucl-th","authors_text":"David Blaschke, Oleksii Ivanytskyi","submitted_at":"2022-05-06T19:24:57Z","abstract_excerpt":"We introduce a family of equations of state (EoS) for hybrid neutron star (NS) matter that is obtained by a two-zone parabolic interpolation between a soft hadronic EoS at low densities and a stiff quark matter EoS with color superconductivity at high densities within a finite region of baryonic chemical potentials $\\mu_B^h < \\mu_B < \\mu_B^q$. We consider two scenarios corresponding to a cross-over and a strong first-order transition between quark and hadron phases considered at finite and zero temperatures. This allows us to analyze the effects of finite entropy on the EoS and mass-radius rel"},"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":"2205.03455","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"nucl-th","submitted_at":"2022-05-06T19:24:57Z","cross_cats_sorted":["astro-ph.HE","hep-ph"],"title_canon_sha256":"acc5752701f2ebd075388190c7f72c14019761691c7f9251a84a0460471c3a8e","abstract_canon_sha256":"bc857b7d0afa988659b95f93637e1ae35d5ceaaf9c84b4f057f4718e98a71d5d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:55:17.266072Z","signature_b64":"sbxL2uyqD+JWmDZ6aWc39DMRjhUQ8MI7M0UtddI77CktykMUVN+8YZzSOlD4/OA9+zL9IJcJaEOMpkGGNewZBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bdd95fb6fa29e7f501171eddac7aefe75b20c53d326f70ed681d35f192111466","last_reissued_at":"2026-07-05T04:55:17.265689Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:55:17.265689Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A new class of hybrid EoS with multiple critical endpoints for simulations of supernovae, neutron stars and their mergers","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"nucl-th","authors_text":"David Blaschke, Oleksii Ivanytskyi","submitted_at":"2022-05-06T19:24:57Z","abstract_excerpt":"We introduce a family of equations of state (EoS) for hybrid neutron star (NS) matter that is obtained by a two-zone parabolic interpolation between a soft hadronic EoS at low densities and a stiff quark matter EoS with color superconductivity at high densities within a finite region of baryonic chemical potentials $\\mu_B^h < \\mu_B < \\mu_B^q$. We consider two scenarios corresponding to a cross-over and a strong first-order transition between quark and hadron phases considered at finite and zero temperatures. This allows us to analyze the effects of finite entropy on the EoS and mass-radius rel"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2205.03455","kind":"arxiv","version":1},"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/2205.03455/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":"2205.03455","created_at":"2026-07-05T04:55:17.265745+00:00"},{"alias_kind":"arxiv_version","alias_value":"2205.03455v1","created_at":"2026-07-05T04:55:17.265745+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2205.03455","created_at":"2026-07-05T04:55:17.265745+00:00"},{"alias_kind":"pith_short_12","alias_value":"XXMV7NX2FHT7","created_at":"2026-07-05T04:55:17.265745+00:00"},{"alias_kind":"pith_short_16","alias_value":"XXMV7NX2FHT7KAIX","created_at":"2026-07-05T04:55:17.265745+00:00"},{"alias_kind":"pith_short_8","alias_value":"XXMV7NX2","created_at":"2026-07-05T04:55:17.265745+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.07758","citing_title":"Fastest spinning millisecond pulsars: indicators for quark matter in neutron stars?","ref_index":59,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45","json":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45.json","graph_json":"https://pith.science/api/pith-number/XXMV7NX2FHT7KAIXD3O2Y6XP45/graph.json","events_json":"https://pith.science/api/pith-number/XXMV7NX2FHT7KAIXD3O2Y6XP45/events.json","paper":"https://pith.science/paper/XXMV7NX2"},"agent_actions":{"view_html":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45","download_json":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45.json","view_paper":"https://pith.science/paper/XXMV7NX2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2205.03455&json=true","fetch_graph":"https://pith.science/api/pith-number/XXMV7NX2FHT7KAIXD3O2Y6XP45/graph.json","fetch_events":"https://pith.science/api/pith-number/XXMV7NX2FHT7KAIXD3O2Y6XP45/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45/action/storage_attestation","attest_author":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45/action/author_attestation","sign_citation":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45/action/citation_signature","submit_replication":"https://pith.science/pith/XXMV7NX2FHT7KAIXD3O2Y6XP45/action/replication_record"}},"created_at":"2026-07-05T04:55:17.265745+00:00","updated_at":"2026-07-05T04:55:17.265745+00:00"}