{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2008:SPDYOXTBGJ2VPM4PWLF5B3DFLG","short_pith_number":"pith:SPDYOXTB","schema_version":"1.0","canonical_sha256":"93c7875e61327557b38fb2cbd0ec6559ba24984604624d425e12806a3b8b35de","source":{"kind":"arxiv","id":"0810.5406","version":1},"attestation_state":"computed","paper":{"title":"Star Formation in Disks: Spiral Arms, Turbulence, and Triggering Mechanisms","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Bruce G. Elmegreen (IBM T.J. Watson Research Center)","submitted_at":"2008-10-30T02:59:19Z","abstract_excerpt":"Star formation is enhanced in spiral arms because of a combination of orbit crowding, cloud collisions, and gravitational instabilities. The characteristic mass for the instability is 10^7 Msun in gas and 10^5 Msun in stars, and the morphology is the familiar beads on a string with 1-2 kpc separation. Similar instabilities occur in resonance rings and tidal tails. Sequential triggering from stellar pressure occurs in two ways. For short times and near distances, it occurs in the bright rims and dense knots that lag behind during cloud dispersal. For long times, it occurs in swept-up shells and"},"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":"0810.5406","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph","submitted_at":"2008-10-30T02:59:19Z","cross_cats_sorted":[],"title_canon_sha256":"8fac36214123b8c9af5feeaf62befe3a85be9c948759a0eb331a4a70a12ff6fb","abstract_canon_sha256":"8c4411553c5c7738a3c58f6529b63fc864087148ef323d2ba0e9c42839facbe5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:15:22.865424Z","signature_b64":"5g06+RbA1UJA/b0uSHknulBkByefhlVWhp4wPtuMmD75+yEfi/sXzlRPRsQERaq3aBJp9NyGrzeFs0/MeJN1AA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"93c7875e61327557b38fb2cbd0ec6559ba24984604624d425e12806a3b8b35de","last_reissued_at":"2026-05-18T02:15:22.864656Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:15:22.864656Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Star Formation in Disks: Spiral Arms, Turbulence, and Triggering Mechanisms","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Bruce G. Elmegreen (IBM T.J. Watson Research Center)","submitted_at":"2008-10-30T02:59:19Z","abstract_excerpt":"Star formation is enhanced in spiral arms because of a combination of orbit crowding, cloud collisions, and gravitational instabilities. The characteristic mass for the instability is 10^7 Msun in gas and 10^5 Msun in stars, and the morphology is the familiar beads on a string with 1-2 kpc separation. Similar instabilities occur in resonance rings and tidal tails. Sequential triggering from stellar pressure occurs in two ways. For short times and near distances, it occurs in the bright rims and dense knots that lag behind during cloud dispersal. For long times, it occurs in swept-up shells and"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0810.5406","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":"0810.5406","created_at":"2026-05-18T02:15:22.864808+00:00"},{"alias_kind":"arxiv_version","alias_value":"0810.5406v1","created_at":"2026-05-18T02:15:22.864808+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0810.5406","created_at":"2026-05-18T02:15:22.864808+00:00"},{"alias_kind":"pith_short_12","alias_value":"SPDYOXTBGJ2V","created_at":"2026-05-18T12:25:58.018023+00:00"},{"alias_kind":"pith_short_16","alias_value":"SPDYOXTBGJ2VPM4P","created_at":"2026-05-18T12:25:58.018023+00:00"},{"alias_kind":"pith_short_8","alias_value":"SPDYOXTB","created_at":"2026-05-18T12:25:58.018023+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.07205","citing_title":"From 2D to 3D: Recovering Turbulent Density Dispersions from Noisy Data","ref_index":10,"is_internal_anchor":true},{"citing_arxiv_id":"2606.10558","citing_title":"Hector Galaxy Survey: Linking the low- and high-mass ends of the initial mass function in star-forming galaxies","ref_index":173,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG","json":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG.json","graph_json":"https://pith.science/api/pith-number/SPDYOXTBGJ2VPM4PWLF5B3DFLG/graph.json","events_json":"https://pith.science/api/pith-number/SPDYOXTBGJ2VPM4PWLF5B3DFLG/events.json","paper":"https://pith.science/paper/SPDYOXTB"},"agent_actions":{"view_html":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG","download_json":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG.json","view_paper":"https://pith.science/paper/SPDYOXTB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0810.5406&json=true","fetch_graph":"https://pith.science/api/pith-number/SPDYOXTBGJ2VPM4PWLF5B3DFLG/graph.json","fetch_events":"https://pith.science/api/pith-number/SPDYOXTBGJ2VPM4PWLF5B3DFLG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG/action/storage_attestation","attest_author":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG/action/author_attestation","sign_citation":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG/action/citation_signature","submit_replication":"https://pith.science/pith/SPDYOXTBGJ2VPM4PWLF5B3DFLG/action/replication_record"}},"created_at":"2026-05-18T02:15:22.864808+00:00","updated_at":"2026-05-18T02:15:22.864808+00:00"}