{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2026:MP5COJWU66CLJNECUPVXJN6AV7","short_pith_number":"pith:MP5COJWU","schema_version":"1.0","canonical_sha256":"63fa2726d4f784b4b482a3eb74b7c0afee518e1b73ac8d21b0c54dc2308df811","source":{"kind":"arxiv","id":"2603.10581","version":2},"attestation_state":"computed","paper":{"title":"The In Situ Growth of Stellar-mass \"Light\" Seed Black Holes in Nuclear Star Clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Norman Murray, Yanlong Shi","submitted_at":"2026-03-11T09:38:01Z","abstract_excerpt":"Remnant black holes (BHs) of massive stars (``light seeds'') are a potential origin for supermassive black holes (SMBHs). We use magnetohydrodynamic simulations to study the formation and growth of light seeds in star-forming giant molecular clouds (GMCs) with masses $10^5$--$10^9\\,M_\\odot$, which evolve for $\\sim 10$--$30\\,\\rm Myr$ and form compact star clusters, akin to high-redshift nuclear star clusters. In particular, the simulations resolve very massive stars (VMSs, 100--$300\\,M_\\odot$), including their radiative and mechanical feedback, and model feedback-regulated accretion onto remnan"},"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":"2603.10581","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2026-03-11T09:38:01Z","cross_cats_sorted":[],"title_canon_sha256":"6d7186cfab3e67e41175e6cf821e6f2e7d535cadd0688e8e03eda4e725245c43","abstract_canon_sha256":"16eab32fcf27d7a0b89e2675aae2bef58c23783c8a3c46c986ae143d382e2eed"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-06-09T02:07:23.709982Z","signature_b64":"/svkkGR8UGaYVTCcsuINGUJ/K5L/paC3e37xtevhFp5X9UM34f5RyWYBITpqO35TEh8VtQshgaLnXEkJnjDYAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"63fa2726d4f784b4b482a3eb74b7c0afee518e1b73ac8d21b0c54dc2308df811","last_reissued_at":"2026-06-09T02:07:23.708849Z","signature_status":"signed_v1","first_computed_at":"2026-06-09T02:07:23.708849Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The In Situ Growth of Stellar-mass \"Light\" Seed Black Holes in Nuclear Star Clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Norman Murray, Yanlong Shi","submitted_at":"2026-03-11T09:38:01Z","abstract_excerpt":"Remnant black holes (BHs) of massive stars (``light seeds'') are a potential origin for supermassive black holes (SMBHs). We use magnetohydrodynamic simulations to study the formation and growth of light seeds in star-forming giant molecular clouds (GMCs) with masses $10^5$--$10^9\\,M_\\odot$, which evolve for $\\sim 10$--$30\\,\\rm Myr$ and form compact star clusters, akin to high-redshift nuclear star clusters. In particular, the simulations resolve very massive stars (VMSs, 100--$300\\,M_\\odot$), including their radiative and mechanical feedback, and model feedback-regulated accretion onto remnan"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2603.10581","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/2603.10581/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":"2603.10581","created_at":"2026-06-09T02:07:23.708970+00:00"},{"alias_kind":"arxiv_version","alias_value":"2603.10581v2","created_at":"2026-06-09T02:07:23.708970+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2603.10581","created_at":"2026-06-09T02:07:23.708970+00:00"},{"alias_kind":"pith_short_12","alias_value":"MP5COJWU66CL","created_at":"2026-06-09T02:07:23.708970+00:00"},{"alias_kind":"pith_short_16","alias_value":"MP5COJWU66CLJNEC","created_at":"2026-06-09T02:07:23.708970+00:00"},{"alias_kind":"pith_short_8","alias_value":"MP5COJWU","created_at":"2026-06-09T02:07:23.708970+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.21593","citing_title":"Predicting intermediate-mass black hole formation in star clusters with machine learning","ref_index":57,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7","json":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7.json","graph_json":"https://pith.science/api/pith-number/MP5COJWU66CLJNECUPVXJN6AV7/graph.json","events_json":"https://pith.science/api/pith-number/MP5COJWU66CLJNECUPVXJN6AV7/events.json","paper":"https://pith.science/paper/MP5COJWU"},"agent_actions":{"view_html":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7","download_json":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7.json","view_paper":"https://pith.science/paper/MP5COJWU","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2603.10581&json=true","fetch_graph":"https://pith.science/api/pith-number/MP5COJWU66CLJNECUPVXJN6AV7/graph.json","fetch_events":"https://pith.science/api/pith-number/MP5COJWU66CLJNECUPVXJN6AV7/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7/action/storage_attestation","attest_author":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7/action/author_attestation","sign_citation":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7/action/citation_signature","submit_replication":"https://pith.science/pith/MP5COJWU66CLJNECUPVXJN6AV7/action/replication_record"}},"created_at":"2026-06-09T02:07:23.708970+00:00","updated_at":"2026-06-09T02:07:23.708970+00:00"}