{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:CVH6VXD56GIE5FIRXYYCQBDEUN","short_pith_number":"pith:CVH6VXD5","schema_version":"1.0","canonical_sha256":"154feadc7df1904e9511be30280464a3558d9b6f49c05237742aba52134457c9","source":{"kind":"arxiv","id":"1407.4103","version":2},"attestation_state":"computed","paper":{"title":"Collapse and dispersal of a homogeneous spin fluid in Einstein-Cartan theory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Amir Hadi Ziaie, Mostafa Hashemi, Shahram Jalalzadeh","submitted_at":"2014-07-15T19:31:16Z","abstract_excerpt":"In the present work, we revisit the process of gravitational collapse of a spherically symmetric homogeneous dust fluid which is known as the Oppenheimer-Snyder (OS) model [1]. We show that such a scenario would not end in a spacetime singularity when the spin degrees of freedom of fermionic particles within the collapsing cloud are taken into account. To this purpose, we take the matter content of the stellar object as a homogeneous Weyssenhoff fluid which is a generalization of perfect fluid in general relativity (GR) to include the spin of matter. Employing the homogeneous and isotropic FLR"},"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":"1407.4103","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2014-07-15T19:31:16Z","cross_cats_sorted":[],"title_canon_sha256":"7a33819174032fb7e187ea05222ef96b0177863a17b45a29b3171344938f3ee2","abstract_canon_sha256":"292cc5d21d3460db02972d351076884ca64bd1e5ce6cebac5b175aaf38333f40"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:26:31.683942Z","signature_b64":"gmlyVV4MQPP7cCWEi7zWIWO6E31tIEVvGzzvQ8e88qPaDkVTWI1e9vbIAI+II8VMobTA2nxIt4kmu2oYOkluBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"154feadc7df1904e9511be30280464a3558d9b6f49c05237742aba52134457c9","last_reissued_at":"2026-05-18T02:26:31.683545Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:26:31.683545Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Collapse and dispersal of a homogeneous spin fluid in Einstein-Cartan theory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Amir Hadi Ziaie, Mostafa Hashemi, Shahram Jalalzadeh","submitted_at":"2014-07-15T19:31:16Z","abstract_excerpt":"In the present work, we revisit the process of gravitational collapse of a spherically symmetric homogeneous dust fluid which is known as the Oppenheimer-Snyder (OS) model [1]. We show that such a scenario would not end in a spacetime singularity when the spin degrees of freedom of fermionic particles within the collapsing cloud are taken into account. To this purpose, we take the matter content of the stellar object as a homogeneous Weyssenhoff fluid which is a generalization of perfect fluid in general relativity (GR) to include the spin of matter. Employing the homogeneous and isotropic FLR"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1407.4103","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":""},"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":"1407.4103","created_at":"2026-05-18T02:26:31.683611+00:00"},{"alias_kind":"arxiv_version","alias_value":"1407.4103v2","created_at":"2026-05-18T02:26:31.683611+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1407.4103","created_at":"2026-05-18T02:26:31.683611+00:00"},{"alias_kind":"pith_short_12","alias_value":"CVH6VXD56GIE","created_at":"2026-05-18T12:28:25.294606+00:00"},{"alias_kind":"pith_short_16","alias_value":"CVH6VXD56GIE5FIR","created_at":"2026-05-18T12:28:25.294606+00:00"},{"alias_kind":"pith_short_8","alias_value":"CVH6VXD5","created_at":"2026-05-18T12:28:25.294606+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2410.19399","citing_title":"Cosmic Dynamics in Einstein-Cartan Theory: Analysing Hubble Tension through Curvature and Torsion field","ref_index":12,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN","json":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN.json","graph_json":"https://pith.science/api/pith-number/CVH6VXD56GIE5FIRXYYCQBDEUN/graph.json","events_json":"https://pith.science/api/pith-number/CVH6VXD56GIE5FIRXYYCQBDEUN/events.json","paper":"https://pith.science/paper/CVH6VXD5"},"agent_actions":{"view_html":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN","download_json":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN.json","view_paper":"https://pith.science/paper/CVH6VXD5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1407.4103&json=true","fetch_graph":"https://pith.science/api/pith-number/CVH6VXD56GIE5FIRXYYCQBDEUN/graph.json","fetch_events":"https://pith.science/api/pith-number/CVH6VXD56GIE5FIRXYYCQBDEUN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN/action/storage_attestation","attest_author":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN/action/author_attestation","sign_citation":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN/action/citation_signature","submit_replication":"https://pith.science/pith/CVH6VXD56GIE5FIRXYYCQBDEUN/action/replication_record"}},"created_at":"2026-05-18T02:26:31.683611+00:00","updated_at":"2026-05-18T02:26:31.683611+00:00"}