{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:C2WOGHGQCB7CXQ6TPNKLAHIGT4","short_pith_number":"pith:C2WOGHGQ","schema_version":"1.0","canonical_sha256":"16ace31cd0107e2bc3d37b54b01d069f236ac0377fc5fb551dde1aa491b830a7","source":{"kind":"arxiv","id":"1809.03499","version":1},"attestation_state":"computed","paper":{"title":"Dynamical cluster disruption and its implications for multiple population models in the E-MOSAICS simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"(2) LJMU), J. M. Diederik Kruijssen (1), Joel L. Pfeffer (2), Marta Reina-Campos (1), Nate Bastian (2), Robert A. Crain (2) ((1) Heidelberg","submitted_at":"2018-09-10T18:00:00Z","abstract_excerpt":"Several models have been advanced to explain the multiple stellar populations observed in globular clusters (GCs). Most models necessitate a large initial population of unenriched stars that provide the pollution for an enriched population, and which are subsequently lost from the cluster. This scenario generally requires clusters to lose $>90$ per cent of their birth mass. We use a suite of 25 cosmological zoom-in simulations of present-day Milky Way-mass galaxies from the \\emosaics project to study whether dynamical disruption by evaporation and tidal shocking provides the necessary mass los"},"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":"1809.03499","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-09-10T18:00:00Z","cross_cats_sorted":[],"title_canon_sha256":"0ba524a09010b4f8ebf3a280a80cf8e069959fac36b4de7d94ae302f8f4c8a2b","abstract_canon_sha256":"9acb3783565c1f2c8fcdf8d3343a6d7157f8da9aa95012125fff66abafe62f5b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:06:00.588138Z","signature_b64":"1sB2cGu2Z7QFeNpp1L9g0OhgLbo3RWNMiZJQvMVrmtSd/hPCN+R5cDNJl4EBkSC1kCVF4OkNwt051H+ofwGjDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"16ace31cd0107e2bc3d37b54b01d069f236ac0377fc5fb551dde1aa491b830a7","last_reissued_at":"2026-05-18T00:06:00.587668Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:06:00.587668Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dynamical cluster disruption and its implications for multiple population models in the E-MOSAICS simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"(2) LJMU), J. M. Diederik Kruijssen (1), Joel L. Pfeffer (2), Marta Reina-Campos (1), Nate Bastian (2), Robert A. Crain (2) ((1) Heidelberg","submitted_at":"2018-09-10T18:00:00Z","abstract_excerpt":"Several models have been advanced to explain the multiple stellar populations observed in globular clusters (GCs). Most models necessitate a large initial population of unenriched stars that provide the pollution for an enriched population, and which are subsequently lost from the cluster. This scenario generally requires clusters to lose $>90$ per cent of their birth mass. We use a suite of 25 cosmological zoom-in simulations of present-day Milky Way-mass galaxies from the \\emosaics project to study whether dynamical disruption by evaporation and tidal shocking provides the necessary mass los"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1809.03499","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":"1809.03499","created_at":"2026-05-18T00:06:00.587745+00:00"},{"alias_kind":"arxiv_version","alias_value":"1809.03499v1","created_at":"2026-05-18T00:06:00.587745+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1809.03499","created_at":"2026-05-18T00:06:00.587745+00:00"},{"alias_kind":"pith_short_12","alias_value":"C2WOGHGQCB7C","created_at":"2026-05-18T12:32:16.446611+00:00"},{"alias_kind":"pith_short_16","alias_value":"C2WOGHGQCB7CXQ6T","created_at":"2026-05-18T12:32:16.446611+00:00"},{"alias_kind":"pith_short_8","alias_value":"C2WOGHGQ","created_at":"2026-05-18T12:32:16.446611+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/C2WOGHGQCB7CXQ6TPNKLAHIGT4","json":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4.json","graph_json":"https://pith.science/api/pith-number/C2WOGHGQCB7CXQ6TPNKLAHIGT4/graph.json","events_json":"https://pith.science/api/pith-number/C2WOGHGQCB7CXQ6TPNKLAHIGT4/events.json","paper":"https://pith.science/paper/C2WOGHGQ"},"agent_actions":{"view_html":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4","download_json":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4.json","view_paper":"https://pith.science/paper/C2WOGHGQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1809.03499&json=true","fetch_graph":"https://pith.science/api/pith-number/C2WOGHGQCB7CXQ6TPNKLAHIGT4/graph.json","fetch_events":"https://pith.science/api/pith-number/C2WOGHGQCB7CXQ6TPNKLAHIGT4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4/action/storage_attestation","attest_author":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4/action/author_attestation","sign_citation":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4/action/citation_signature","submit_replication":"https://pith.science/pith/C2WOGHGQCB7CXQ6TPNKLAHIGT4/action/replication_record"}},"created_at":"2026-05-18T00:06:00.587745+00:00","updated_at":"2026-05-18T00:06:00.587745+00:00"}