{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:W63P6QEJQLNZ76UV7BVLCSCCLO","short_pith_number":"pith:W63P6QEJ","schema_version":"1.0","canonical_sha256":"b7b6ff408982db9ffa95f86ab148425b88e499af0934ae253af0f811408ed6c7","source":{"kind":"arxiv","id":"1002.4401","version":1},"attestation_state":"computed","paper":{"title":"Properties of hierarchically forming star clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2), Astronomy, Bonn (3) School of Physics, Cambridge (2) Argelander-Institut, C.J. Clarke (1), I.A. Bonnell (3), P. Kroupa (2) ( (1) Institute of Astronomy, St. Andrews), Th. Maschberger (1","submitted_at":"2010-02-23T20:03:47Z","abstract_excerpt":"We undertake a systematic analysis of the early (< 0.5 Myr) evolution of clustering and the stellar initial mass function in turbulent fragmentation simulations. These large scale simulations for the first time offer the opportunity for a statistical analysis of IMF variations and correlations between stellar properties and cluster richness. The typical evolutionary scenario involves star formation in small-n clusters which then progressively merge; the first stars to form are seeds of massive stars and achieve a headstart in mass acquisition. These massive seeds end up in the cores of cluster"},"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":"1002.4401","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2010-02-23T20:03:47Z","cross_cats_sorted":[],"title_canon_sha256":"4efb75dce46fc762465bd9956a9f7e31829cd25c9d80960d01715eca7bea307a","abstract_canon_sha256":"02deb31f4ad64c0259d9275864b881cd4f0d1ce4aae3554273d50cfb55b79f94"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:08:57.662350Z","signature_b64":"KLaOh/aT64+XxfbSNBUnju4wLMdQSHgaoPcA97zo3cxtvshydY59kcesWOcufOHhf9too+nCK7sEga3Fq+rfAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b7b6ff408982db9ffa95f86ab148425b88e499af0934ae253af0f811408ed6c7","last_reissued_at":"2026-05-18T02:08:57.661676Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:08:57.661676Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Properties of hierarchically forming star clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2), Astronomy, Bonn (3) School of Physics, Cambridge (2) Argelander-Institut, C.J. Clarke (1), I.A. Bonnell (3), P. Kroupa (2) ( (1) Institute of Astronomy, St. Andrews), Th. Maschberger (1","submitted_at":"2010-02-23T20:03:47Z","abstract_excerpt":"We undertake a systematic analysis of the early (< 0.5 Myr) evolution of clustering and the stellar initial mass function in turbulent fragmentation simulations. These large scale simulations for the first time offer the opportunity for a statistical analysis of IMF variations and correlations between stellar properties and cluster richness. The typical evolutionary scenario involves star formation in small-n clusters which then progressively merge; the first stars to form are seeds of massive stars and achieve a headstart in mass acquisition. These massive seeds end up in the cores of cluster"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1002.4401","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":""},"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":"1002.4401","created_at":"2026-05-18T02:08:57.661776+00:00"},{"alias_kind":"arxiv_version","alias_value":"1002.4401v1","created_at":"2026-05-18T02:08:57.661776+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1002.4401","created_at":"2026-05-18T02:08:57.661776+00:00"},{"alias_kind":"pith_short_12","alias_value":"W63P6QEJQLNZ","created_at":"2026-05-18T12:26:15.391820+00:00"},{"alias_kind":"pith_short_16","alias_value":"W63P6QEJQLNZ76UV","created_at":"2026-05-18T12:26:15.391820+00:00"},{"alias_kind":"pith_short_8","alias_value":"W63P6QEJ","created_at":"2026-05-18T12:26:15.391820+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO","json":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO.json","graph_json":"https://pith.science/api/pith-number/W63P6QEJQLNZ76UV7BVLCSCCLO/graph.json","events_json":"https://pith.science/api/pith-number/W63P6QEJQLNZ76UV7BVLCSCCLO/events.json","paper":"https://pith.science/paper/W63P6QEJ"},"agent_actions":{"view_html":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO","download_json":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO.json","view_paper":"https://pith.science/paper/W63P6QEJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1002.4401&json=true","fetch_graph":"https://pith.science/api/pith-number/W63P6QEJQLNZ76UV7BVLCSCCLO/graph.json","fetch_events":"https://pith.science/api/pith-number/W63P6QEJQLNZ76UV7BVLCSCCLO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO/action/storage_attestation","attest_author":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO/action/author_attestation","sign_citation":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO/action/citation_signature","submit_replication":"https://pith.science/pith/W63P6QEJQLNZ76UV7BVLCSCCLO/action/replication_record"}},"created_at":"2026-05-18T02:08:57.661776+00:00","updated_at":"2026-05-18T02:08:57.661776+00:00"}