{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:KHANAMSPCTLFLVBSMOZHE75MBF","short_pith_number":"pith:KHANAMSP","schema_version":"1.0","canonical_sha256":"51c0d0324f14d655d43263b2727fac0958c7a14b9b585929e2a48028394df7ff","source":{"kind":"arxiv","id":"1411.3002","version":1},"attestation_state":"computed","paper":{"title":"Primordial mass segregation in simulations of star formation?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"2. Excellence Cluster, 3) (1. Liverpool John Moores University, 3. USM, Barbara Ercolano (2, Garching, Germany, Germany), James E. Dale (2), Munich, Richard J. Parker (1), UK","submitted_at":"2014-11-11T22:01:15Z","abstract_excerpt":"We take the end result of smoothed particle hydrodynamics (SPH) simulations of star formation which include feedback from photoionisation and stellar winds and evolve them for a further 10Myr using $N$-body simulations. We compare the evolution of each simulation to a control run without feedback, and to a run with photoionisation feedback only. In common with previous work, we find that the presence of feedback prevents the runaway growth of massive stars, and the resulting star-forming regions are less dense, and preserve their initial substructure for longer. The addition of stellar winds t"},"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":"1411.3002","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2014-11-11T22:01:15Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"e2de798845aa5aa1b6e433a2cf5230b75deceb2896c91f2471012c53224669ae","abstract_canon_sha256":"78a4cb609e29043969c8c45b7c8a202f2c54d5216e66460b76c8e3f985561b00"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:41:31.430127Z","signature_b64":"VLFAzm6NDpGAFbPDYGFe5b/9tXXgJJ3uw8g0DdJYNHryUTCSLgHUIech7y8dnHpNab6hMgv08A94hmZTWDQGCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"51c0d0324f14d655d43263b2727fac0958c7a14b9b585929e2a48028394df7ff","last_reissued_at":"2026-05-18T01:41:31.429287Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:41:31.429287Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Primordial mass segregation in simulations of star formation?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"2. Excellence Cluster, 3) (1. Liverpool John Moores University, 3. USM, Barbara Ercolano (2, Garching, Germany, Germany), James E. Dale (2), Munich, Richard J. Parker (1), UK","submitted_at":"2014-11-11T22:01:15Z","abstract_excerpt":"We take the end result of smoothed particle hydrodynamics (SPH) simulations of star formation which include feedback from photoionisation and stellar winds and evolve them for a further 10Myr using $N$-body simulations. We compare the evolution of each simulation to a control run without feedback, and to a run with photoionisation feedback only. In common with previous work, we find that the presence of feedback prevents the runaway growth of massive stars, and the resulting star-forming regions are less dense, and preserve their initial substructure for longer. The addition of stellar winds t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1411.3002","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":"1411.3002","created_at":"2026-05-18T01:41:31.429436+00:00"},{"alias_kind":"arxiv_version","alias_value":"1411.3002v1","created_at":"2026-05-18T01:41:31.429436+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1411.3002","created_at":"2026-05-18T01:41:31.429436+00:00"},{"alias_kind":"pith_short_12","alias_value":"KHANAMSPCTLF","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_16","alias_value":"KHANAMSPCTLFLVBS","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_8","alias_value":"KHANAMSP","created_at":"2026-05-18T12:28:35.611951+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/KHANAMSPCTLFLVBSMOZHE75MBF","json":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF.json","graph_json":"https://pith.science/api/pith-number/KHANAMSPCTLFLVBSMOZHE75MBF/graph.json","events_json":"https://pith.science/api/pith-number/KHANAMSPCTLFLVBSMOZHE75MBF/events.json","paper":"https://pith.science/paper/KHANAMSP"},"agent_actions":{"view_html":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF","download_json":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF.json","view_paper":"https://pith.science/paper/KHANAMSP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1411.3002&json=true","fetch_graph":"https://pith.science/api/pith-number/KHANAMSPCTLFLVBSMOZHE75MBF/graph.json","fetch_events":"https://pith.science/api/pith-number/KHANAMSPCTLFLVBSMOZHE75MBF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF/action/storage_attestation","attest_author":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF/action/author_attestation","sign_citation":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF/action/citation_signature","submit_replication":"https://pith.science/pith/KHANAMSPCTLFLVBSMOZHE75MBF/action/replication_record"}},"created_at":"2026-05-18T01:41:31.429436+00:00","updated_at":"2026-05-18T01:41:31.429436+00:00"}