{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:RUVH4JP4CUFFQVWDDKPYPES37D","short_pith_number":"pith:RUVH4JP4","schema_version":"1.0","canonical_sha256":"8d2a7e25fc150a5856c31a9f87925bf8f5c47fa6b0e05b2d18990e1c2c631978","source":{"kind":"arxiv","id":"1404.4630","version":2},"attestation_state":"computed","paper":{"title":"Formation of an embryonic supermassive star in the first galaxy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Elizabeth J. Tasker, Kazuyuki Omukai, Kohei Inayoshi","submitted_at":"2014-04-17T20:00:00Z","abstract_excerpt":"We studied the gravitational collapse of a warm (~8000 K) primordial-gas cloud as a candidate progenitor for a supermassive star (SMS; >10^5 Msun) using a three-dimensional hydrodynamical simulation, including all the relevant cooling processes of both H_2 and H, which can potentially induce cloud fragmentation. This is the first simulation of this kind to resolve protostar formation. We find that the cloud undergoes runaway collapse without a major episode of fragmentation. Although the H_2 fraction jumps by a large factor via the three-body reaction at ~10^-13 g/cm^3, its cooling remains ine"},"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":"1404.4630","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2014-04-17T20:00:00Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"0e0b7df6529056467d4620592b77ce49bab9e1fcdaa4f75e3b6d30b389569b77","abstract_canon_sha256":"5bcda37136a91df4d210277610ef1559728a28aa6973bda45a8127e55a0a2ca0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:43:28.773994Z","signature_b64":"7jxfx9BXvRBUMPnSZ/pelYyXIpanVhnB85dg8lMGkEm2LHwqt5t7E5c2+KNigUFexM46fThJdevlcOyj1gYoBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8d2a7e25fc150a5856c31a9f87925bf8f5c47fa6b0e05b2d18990e1c2c631978","last_reissued_at":"2026-05-18T01:43:28.773354Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:43:28.773354Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Formation of an embryonic supermassive star in the first galaxy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Elizabeth J. Tasker, Kazuyuki Omukai, Kohei Inayoshi","submitted_at":"2014-04-17T20:00:00Z","abstract_excerpt":"We studied the gravitational collapse of a warm (~8000 K) primordial-gas cloud as a candidate progenitor for a supermassive star (SMS; >10^5 Msun) using a three-dimensional hydrodynamical simulation, including all the relevant cooling processes of both H_2 and H, which can potentially induce cloud fragmentation. This is the first simulation of this kind to resolve protostar formation. We find that the cloud undergoes runaway collapse without a major episode of fragmentation. Although the H_2 fraction jumps by a large factor via the three-body reaction at ~10^-13 g/cm^3, its cooling remains ine"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1404.4630","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":"1404.4630","created_at":"2026-05-18T01:43:28.773443+00:00"},{"alias_kind":"arxiv_version","alias_value":"1404.4630v2","created_at":"2026-05-18T01:43:28.773443+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1404.4630","created_at":"2026-05-18T01:43:28.773443+00:00"},{"alias_kind":"pith_short_12","alias_value":"RUVH4JP4CUFF","created_at":"2026-05-18T12:28:46.137349+00:00"},{"alias_kind":"pith_short_16","alias_value":"RUVH4JP4CUFFQVWD","created_at":"2026-05-18T12:28:46.137349+00:00"},{"alias_kind":"pith_short_8","alias_value":"RUVH4JP4","created_at":"2026-05-18T12:28:46.137349+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2509.25325","citing_title":"Direct Collapse Black Hole Candidates from Decaying Dark Matter","ref_index":64,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D","json":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D.json","graph_json":"https://pith.science/api/pith-number/RUVH4JP4CUFFQVWDDKPYPES37D/graph.json","events_json":"https://pith.science/api/pith-number/RUVH4JP4CUFFQVWDDKPYPES37D/events.json","paper":"https://pith.science/paper/RUVH4JP4"},"agent_actions":{"view_html":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D","download_json":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D.json","view_paper":"https://pith.science/paper/RUVH4JP4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1404.4630&json=true","fetch_graph":"https://pith.science/api/pith-number/RUVH4JP4CUFFQVWDDKPYPES37D/graph.json","fetch_events":"https://pith.science/api/pith-number/RUVH4JP4CUFFQVWDDKPYPES37D/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D/action/storage_attestation","attest_author":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D/action/author_attestation","sign_citation":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D/action/citation_signature","submit_replication":"https://pith.science/pith/RUVH4JP4CUFFQVWDDKPYPES37D/action/replication_record"}},"created_at":"2026-05-18T01:43:28.773443+00:00","updated_at":"2026-05-18T01:43:28.773443+00:00"}