{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1998:5TB7TQISFBE7F5MVZH2KWUKIAL","short_pith_number":"pith:5TB7TQIS","schema_version":"1.0","canonical_sha256":"ecc3f9c1122849f2f595c9f4ab514802d9e9913c2735a7b6059073bbcf5a70a5","source":{"kind":"arxiv","id":"astro-ph/9810397","version":1},"attestation_state":"computed","paper":{"title":"Collapse of a Molecular Cloud Core to Stellar Densities: The First Three-Dimensional Calculations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Matthew R. Bate","submitted_at":"1998-10-24T12:44:00Z","abstract_excerpt":"We present results from the first three-dimensional calculations ever to follow the collapse of a molecular cloud core (~ 10^{-18} g cm^{-3}) to stellar densities (> 0.01 g cm^{-3}). The calculations resolve structures over 7 orders of magnitude in spatial extent (~ 5000 AU - 0.1 R_\\odot), and over 17 orders of magnitude in density contrast. With these calculations, we consider whether fragmentation to form a close binary stellar system can occur during the second collapse phase. We find that, if the quasistatic core that forms before the second collapse phase is dynamically unstable to the gr"},"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":"astro-ph/9810397","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1998-10-24T12:44:00Z","cross_cats_sorted":[],"title_canon_sha256":"b9b07b52a6460a262177b66ade4dcd1b24a25a0e6737a27d451802b2712f055c","abstract_canon_sha256":"8be0286d68f88490a1872ac820d1647de3db350bd729f0b3819ff467faecb18d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:07:08.407804Z","signature_b64":"MTEIV7DSFqUgiWagoENprJx3/sYTIEUC77mrj4G0fvMWgZPSG5Zopo+uRbEI6KI52fl322qc8hKvP+G2XOtuBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ecc3f9c1122849f2f595c9f4ab514802d9e9913c2735a7b6059073bbcf5a70a5","last_reissued_at":"2026-07-04T16:07:08.407465Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:07:08.407465Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Collapse of a Molecular Cloud Core to Stellar Densities: The First Three-Dimensional Calculations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Matthew R. Bate","submitted_at":"1998-10-24T12:44:00Z","abstract_excerpt":"We present results from the first three-dimensional calculations ever to follow the collapse of a molecular cloud core (~ 10^{-18} g cm^{-3}) to stellar densities (> 0.01 g cm^{-3}). The calculations resolve structures over 7 orders of magnitude in spatial extent (~ 5000 AU - 0.1 R_\\odot), and over 17 orders of magnitude in density contrast. With these calculations, we consider whether fragmentation to form a close binary stellar system can occur during the second collapse phase. We find that, if the quasistatic core that forms before the second collapse phase is dynamically unstable to the gr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9810397","kind":"arxiv","version":1},"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/astro-ph/9810397/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":"astro-ph/9810397","created_at":"2026-07-04T16:07:08.407515+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9810397v1","created_at":"2026-07-04T16:07:08.407515+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9810397","created_at":"2026-07-04T16:07:08.407515+00:00"},{"alias_kind":"pith_short_12","alias_value":"5TB7TQISFBE7","created_at":"2026-07-04T16:07:08.407515+00:00"},{"alias_kind":"pith_short_16","alias_value":"5TB7TQISFBE7F5MV","created_at":"2026-07-04T16:07:08.407515+00:00"},{"alias_kind":"pith_short_8","alias_value":"5TB7TQIS","created_at":"2026-07-04T16:07:08.407515+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.23794","citing_title":"MINDS: Complementary inclinations in the binary system HK Tau reveal gas- and ice-phase chemistry","ref_index":73,"is_internal_anchor":true},{"citing_arxiv_id":"2605.23469","citing_title":"TOI-7154b: A Close-in Massive Brown Dwarf in an Eccentric Orbit","ref_index":145,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL","json":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL.json","graph_json":"https://pith.science/api/pith-number/5TB7TQISFBE7F5MVZH2KWUKIAL/graph.json","events_json":"https://pith.science/api/pith-number/5TB7TQISFBE7F5MVZH2KWUKIAL/events.json","paper":"https://pith.science/paper/5TB7TQIS"},"agent_actions":{"view_html":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL","download_json":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL.json","view_paper":"https://pith.science/paper/5TB7TQIS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9810397&json=true","fetch_graph":"https://pith.science/api/pith-number/5TB7TQISFBE7F5MVZH2KWUKIAL/graph.json","fetch_events":"https://pith.science/api/pith-number/5TB7TQISFBE7F5MVZH2KWUKIAL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL/action/storage_attestation","attest_author":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL/action/author_attestation","sign_citation":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL/action/citation_signature","submit_replication":"https://pith.science/pith/5TB7TQISFBE7F5MVZH2KWUKIAL/action/replication_record"}},"created_at":"2026-07-04T16:07:08.407515+00:00","updated_at":"2026-07-04T16:07:08.407515+00:00"}