{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:ZCSK7NT57BYJTFHPEM5FWBVCUB","short_pith_number":"pith:ZCSK7NT5","schema_version":"1.0","canonical_sha256":"c8a4afb67df8709994ef233a5b06a2a05c77a7c6dc87382c1a00b04ceaad20d8","source":{"kind":"arxiv","id":"2007.03436","version":2},"attestation_state":"computed","paper":{"title":"Why can hadronic stars convert into strange quark stars with larger radii","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"nucl-th","authors_text":"Alessandro Drago, Giuseppe Pagliara","submitted_at":"2020-07-01T09:27:26Z","abstract_excerpt":"The total binding energy of compact stars is the sum of the gravitational binding energy $(BE)_g$ and the nuclear binding energy $(BE)_n$, the last being related to the microphysics of the interactions. While the first is positive (binding) both for hadronic stars and for strange quark stars, the second is large and negative for hadronic stars (anti-binding) and either small and negative (anti-binding) or positive (binding) for strange quark stars. A hadronic star can convert into a strange quark star with a larger radius because the consequent reduction of $(BE)_g$ is over-compensated by the "},"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":"2007.03436","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2020-07-01T09:27:26Z","cross_cats_sorted":["astro-ph.HE","hep-ph"],"title_canon_sha256":"7289da7994d2c9c410b4e217d7fc1fecd4ef69c552113eaa774e6cf44d89a992","abstract_canon_sha256":"3d9db8c7425ea3f7dcd110fc1a55ef5e67955cd9fe598132f7acdee12fe0787f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:48:28.473888Z","signature_b64":"+J9y8f7AUAO8Wez7VVLbFE9E7zXmvX1sVs4bH9Xz2ZyXYvB7Li2g/x3MhZA4NiDoPIa6l/63yqW24nHT7+xnCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c8a4afb67df8709994ef233a5b06a2a05c77a7c6dc87382c1a00b04ceaad20d8","last_reissued_at":"2026-07-05T01:48:28.473456Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:48:28.473456Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Why can hadronic stars convert into strange quark stars with larger radii","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","hep-ph"],"primary_cat":"nucl-th","authors_text":"Alessandro Drago, Giuseppe Pagliara","submitted_at":"2020-07-01T09:27:26Z","abstract_excerpt":"The total binding energy of compact stars is the sum of the gravitational binding energy $(BE)_g$ and the nuclear binding energy $(BE)_n$, the last being related to the microphysics of the interactions. While the first is positive (binding) both for hadronic stars and for strange quark stars, the second is large and negative for hadronic stars (anti-binding) and either small and negative (anti-binding) or positive (binding) for strange quark stars. A hadronic star can convert into a strange quark star with a larger radius because the consequent reduction of $(BE)_g$ is over-compensated by the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2007.03436","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/2007.03436/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":"2007.03436","created_at":"2026-07-05T01:48:28.473521+00:00"},{"alias_kind":"arxiv_version","alias_value":"2007.03436v2","created_at":"2026-07-05T01:48:28.473521+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2007.03436","created_at":"2026-07-05T01:48:28.473521+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZCSK7NT57BYJ","created_at":"2026-07-05T01:48:28.473521+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZCSK7NT57BYJTFHP","created_at":"2026-07-05T01:48:28.473521+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZCSK7NT5","created_at":"2026-07-05T01:48:28.473521+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.15222","citing_title":"Explainable autoencoder for neutron star dense matter parameter estimation","ref_index":55,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB","json":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB.json","graph_json":"https://pith.science/api/pith-number/ZCSK7NT57BYJTFHPEM5FWBVCUB/graph.json","events_json":"https://pith.science/api/pith-number/ZCSK7NT57BYJTFHPEM5FWBVCUB/events.json","paper":"https://pith.science/paper/ZCSK7NT5"},"agent_actions":{"view_html":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB","download_json":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB.json","view_paper":"https://pith.science/paper/ZCSK7NT5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2007.03436&json=true","fetch_graph":"https://pith.science/api/pith-number/ZCSK7NT57BYJTFHPEM5FWBVCUB/graph.json","fetch_events":"https://pith.science/api/pith-number/ZCSK7NT57BYJTFHPEM5FWBVCUB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB/action/storage_attestation","attest_author":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB/action/author_attestation","sign_citation":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB/action/citation_signature","submit_replication":"https://pith.science/pith/ZCSK7NT57BYJTFHPEM5FWBVCUB/action/replication_record"}},"created_at":"2026-07-05T01:48:28.473521+00:00","updated_at":"2026-07-05T01:48:28.473521+00:00"}