{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:UZQNTWB73AHUNF2MI63DX6NYTN","short_pith_number":"pith:UZQNTWB7","schema_version":"1.0","canonical_sha256":"a660d9d83fd80f46974c47b63bf9b89b6b3a422f7969386e41fdc5b34533e879","source":{"kind":"arxiv","id":"1512.03834","version":2},"attestation_state":"computed","paper":{"title":"Are the Formation and Abundances of Metal-Poor Stars the Result of Dust Dynamics?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Charlie Conroy (Harvard), Philip F. Hopkins (Caltech)","submitted_at":"2015-12-11T21:33:43Z","abstract_excerpt":"Large dust grains can fluctuate dramatically in their local density, relative to gas, in neutral, turbulent disks. Small, high-redshift galaxies (before reionization) represent ideal environments for this process. We show via simple arguments and simulations that order-of-magnitude fluctuations are expected in local abundances of large grains under these conditions. This can have important consequences for star formation and stellar abundances in extremely metal-poor stars. Low-mass stars could form in dust-enhanced regions almost immediately after some dust forms, even if the galaxy-average m"},"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":"1512.03834","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2015-12-11T21:33:43Z","cross_cats_sorted":["astro-ph.CO","astro-ph.SR"],"title_canon_sha256":"a416f159880f73bca3fc778e6ca0205d59d525eebd8fa3e833702544b4f64ab0","abstract_canon_sha256":"38690899ecd2e7d523b45953bb79291e91f004c505e91c02599b2e7ca84695ea"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:40:41.579241Z","signature_b64":"Y5rHSV9uG03Y5aLmXwzPU/kRQ4I6AHDLtcEPUrPUCZf+N8uH7oMz9akNEb8q5aGAeluYta5EXTX+yk6EQPjVDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a660d9d83fd80f46974c47b63bf9b89b6b3a422f7969386e41fdc5b34533e879","last_reissued_at":"2026-05-18T00:40:41.578573Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:40:41.578573Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Are the Formation and Abundances of Metal-Poor Stars the Result of Dust Dynamics?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.SR"],"primary_cat":"astro-ph.GA","authors_text":"Charlie Conroy (Harvard), Philip F. Hopkins (Caltech)","submitted_at":"2015-12-11T21:33:43Z","abstract_excerpt":"Large dust grains can fluctuate dramatically in their local density, relative to gas, in neutral, turbulent disks. Small, high-redshift galaxies (before reionization) represent ideal environments for this process. We show via simple arguments and simulations that order-of-magnitude fluctuations are expected in local abundances of large grains under these conditions. This can have important consequences for star formation and stellar abundances in extremely metal-poor stars. Low-mass stars could form in dust-enhanced regions almost immediately after some dust forms, even if the galaxy-average m"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1512.03834","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":""},"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":"1512.03834","created_at":"2026-05-18T00:40:41.578685+00:00"},{"alias_kind":"arxiv_version","alias_value":"1512.03834v2","created_at":"2026-05-18T00:40:41.578685+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1512.03834","created_at":"2026-05-18T00:40:41.578685+00:00"},{"alias_kind":"pith_short_12","alias_value":"UZQNTWB73AHU","created_at":"2026-05-18T12:29:44.643036+00:00"},{"alias_kind":"pith_short_16","alias_value":"UZQNTWB73AHUNF2M","created_at":"2026-05-18T12:29:44.643036+00:00"},{"alias_kind":"pith_short_8","alias_value":"UZQNTWB7","created_at":"2026-05-18T12:29:44.643036+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/UZQNTWB73AHUNF2MI63DX6NYTN","json":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN.json","graph_json":"https://pith.science/api/pith-number/UZQNTWB73AHUNF2MI63DX6NYTN/graph.json","events_json":"https://pith.science/api/pith-number/UZQNTWB73AHUNF2MI63DX6NYTN/events.json","paper":"https://pith.science/paper/UZQNTWB7"},"agent_actions":{"view_html":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN","download_json":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN.json","view_paper":"https://pith.science/paper/UZQNTWB7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1512.03834&json=true","fetch_graph":"https://pith.science/api/pith-number/UZQNTWB73AHUNF2MI63DX6NYTN/graph.json","fetch_events":"https://pith.science/api/pith-number/UZQNTWB73AHUNF2MI63DX6NYTN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN/action/storage_attestation","attest_author":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN/action/author_attestation","sign_citation":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN/action/citation_signature","submit_replication":"https://pith.science/pith/UZQNTWB73AHUNF2MI63DX6NYTN/action/replication_record"}},"created_at":"2026-05-18T00:40:41.578685+00:00","updated_at":"2026-05-18T00:40:41.578685+00:00"}