{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:X25OCCEAWIJDY2AF5JOQVCFN7N","short_pith_number":"pith:X25OCCEA","schema_version":"1.0","canonical_sha256":"bebae10880b2123c6805ea5d0a88adfb58db16dff6790091bffd90d14249579a","source":{"kind":"arxiv","id":"2009.12571","version":3},"attestation_state":"computed","paper":{"title":"Bayesian inference of quark star equation of state using the NICER PSR J0030+0451 data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ang Li, Jin-Liang Jiang, Ren-Xin Xu, Shao-Peng Tang, Zhi-Qiang Miao","submitted_at":"2020-09-26T11:30:31Z","abstract_excerpt":"We constrain the equation of state of quark stars within the Bayesian statistical approach using the mass and radius measurements of PSR J0030+0451 from NICER. Three types of bag models, with and without non-zero finite quark mass and/or superfluidity, are employed for quark stars made up with self-bound strange quark matter. We find the $90\\%$ posterior credible boundary around the most probable values of the quark star maximum mass is $M_{\\rm TOV}=2.38_{-0.23}^{+0.26}\\,M_{\\odot}$, within the model flexibility of the finite quark mass, the quark pairing gap, and the perturbative contribution "},"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":"2009.12571","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2020-09-26T11:30:31Z","cross_cats_sorted":["astro-ph.SR","nucl-th"],"title_canon_sha256":"527f2008db14778e8a876d3f9d2bf67b93479471fe2c57980429edf582402cdf","abstract_canon_sha256":"3eca3da0924d08dd3d43b19b7ab30f1b64155fce3848c792cf0a1c4cf15ba291"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:06:57.526568Z","signature_b64":"+gFkLoj1Eim+5/fI95wcSqnD1I8LRtRW9DlZW0YnR0Wa4bc4QRbpJJbZADdNz9DIP8PDLli1hvCNG+G6jASKBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bebae10880b2123c6805ea5d0a88adfb58db16dff6790091bffd90d14249579a","last_reissued_at":"2026-07-05T03:06:57.526093Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:06:57.526093Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Bayesian inference of quark star equation of state using the NICER PSR J0030+0451 data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ang Li, Jin-Liang Jiang, Ren-Xin Xu, Shao-Peng Tang, Zhi-Qiang Miao","submitted_at":"2020-09-26T11:30:31Z","abstract_excerpt":"We constrain the equation of state of quark stars within the Bayesian statistical approach using the mass and radius measurements of PSR J0030+0451 from NICER. Three types of bag models, with and without non-zero finite quark mass and/or superfluidity, are employed for quark stars made up with self-bound strange quark matter. We find the $90\\%$ posterior credible boundary around the most probable values of the quark star maximum mass is $M_{\\rm TOV}=2.38_{-0.23}^{+0.26}\\,M_{\\odot}$, within the model flexibility of the finite quark mass, the quark pairing gap, and the perturbative contribution "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2009.12571","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/2009.12571/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":"2009.12571","created_at":"2026-07-05T03:06:57.526153+00:00"},{"alias_kind":"arxiv_version","alias_value":"2009.12571v3","created_at":"2026-07-05T03:06:57.526153+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2009.12571","created_at":"2026-07-05T03:06:57.526153+00:00"},{"alias_kind":"pith_short_12","alias_value":"X25OCCEAWIJD","created_at":"2026-07-05T03:06:57.526153+00:00"},{"alias_kind":"pith_short_16","alias_value":"X25OCCEAWIJDY2AF","created_at":"2026-07-05T03:06:57.526153+00:00"},{"alias_kind":"pith_short_8","alias_value":"X25OCCEA","created_at":"2026-07-05T03:06:57.526153+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"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":93,"is_internal_anchor":false},{"citing_arxiv_id":"2510.22137","citing_title":"Inferring neutron-star Love-Q relations from gravitational waves in the hierarchical Bayesian framework","ref_index":35,"is_internal_anchor":false},{"citing_arxiv_id":"2105.06979","citing_title":"The Radius of PSR J0740+6620 from NICER and XMM-Newton Data","ref_index":73,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N","json":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N.json","graph_json":"https://pith.science/api/pith-number/X25OCCEAWIJDY2AF5JOQVCFN7N/graph.json","events_json":"https://pith.science/api/pith-number/X25OCCEAWIJDY2AF5JOQVCFN7N/events.json","paper":"https://pith.science/paper/X25OCCEA"},"agent_actions":{"view_html":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N","download_json":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N.json","view_paper":"https://pith.science/paper/X25OCCEA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2009.12571&json=true","fetch_graph":"https://pith.science/api/pith-number/X25OCCEAWIJDY2AF5JOQVCFN7N/graph.json","fetch_events":"https://pith.science/api/pith-number/X25OCCEAWIJDY2AF5JOQVCFN7N/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N/action/timestamp_anchor","attest_storage":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N/action/storage_attestation","attest_author":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N/action/author_attestation","sign_citation":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N/action/citation_signature","submit_replication":"https://pith.science/pith/X25OCCEAWIJDY2AF5JOQVCFN7N/action/replication_record"}},"created_at":"2026-07-05T03:06:57.526153+00:00","updated_at":"2026-07-05T03:06:57.526153+00:00"}