{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:RPHDKHDACOZFWX53TKSNGQWFDO","short_pith_number":"pith:RPHDKHDA","schema_version":"1.0","canonical_sha256":"8bce351c6013b25b5fbb9aa4d342c51bb94d275c4e067af525b852c90ad0cedb","source":{"kind":"arxiv","id":"astro-ph/0605120","version":2},"attestation_state":"computed","paper":{"title":"Simulating the formation of molecular clouds. I. Slow formation by gravitational collapse from static initial conditions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), (2) AMNH), M.-M. Mac Low (2) ((1) Astrophysikalisches Institut Potsdam, S. C. O. Glover (1","submitted_at":"2006-05-04T10:04:41Z","abstract_excerpt":"We study the formation of H2 in the ISM, using a modified version of the astrophysical magnetohydrodynamical code ZEUS-MP that includes a non-equilibrium treatment of the formation and destruction of H2. We examine two different approximations to treat the shielding of H2 against photodissociation: a local approximation, which gives us a solid lower bound on the amount of shielding, and a method based on ray-tracing that is considerably more accurate in some circumstances but that produces results that are harder to clearly interpret. Either approximation allows one to perform three-dimensiona"},"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":"astro-ph/0605120","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-05-04T10:04:41Z","cross_cats_sorted":[],"title_canon_sha256":"9b0e91db842b47da6e938f803f2fcd1ddfcedebb7b6af8e06a8b1ebe12fa0c4c","abstract_canon_sha256":"1c71b4648d5459407792e50b78c9f647c19bb962e5b9876b20fcae8258147eef"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:22:18.935776Z","signature_b64":"4QcqBBeD5RIvZKaxFdAUagLjnwYiYTOSFMHxTPoigjS68jHqT4paLFTuOeoQBpf2pS3s99hrGTlhSBa0DE6TAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8bce351c6013b25b5fbb9aa4d342c51bb94d275c4e067af525b852c90ad0cedb","last_reissued_at":"2026-07-04T15:22:18.935386Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:22:18.935386Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulating the formation of molecular clouds. I. Slow formation by gravitational collapse from static initial conditions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2), (2) AMNH), M.-M. Mac Low (2) ((1) Astrophysikalisches Institut Potsdam, S. C. O. Glover (1","submitted_at":"2006-05-04T10:04:41Z","abstract_excerpt":"We study the formation of H2 in the ISM, using a modified version of the astrophysical magnetohydrodynamical code ZEUS-MP that includes a non-equilibrium treatment of the formation and destruction of H2. We examine two different approximations to treat the shielding of H2 against photodissociation: a local approximation, which gives us a solid lower bound on the amount of shielding, and a method based on ray-tracing that is considerably more accurate in some circumstances but that produces results that are harder to clearly interpret. Either approximation allows one to perform three-dimensiona"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0605120","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0605120/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"astro-ph/0605120","created_at":"2026-07-04T15:22:18.935444+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0605120v2","created_at":"2026-07-04T15:22:18.935444+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0605120","created_at":"2026-07-04T15:22:18.935444+00:00"},{"alias_kind":"pith_short_12","alias_value":"RPHDKHDACOZF","created_at":"2026-07-04T15:22:18.935444+00:00"},{"alias_kind":"pith_short_16","alias_value":"RPHDKHDACOZFWX53","created_at":"2026-07-04T15:22:18.935444+00:00"},{"alias_kind":"pith_short_8","alias_value":"RPHDKHDA","created_at":"2026-07-04T15:22:18.935444+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.01338","citing_title":"IRIS: Deciphering Spectral-Line Imagery of the Galactic Center by Machine-Learning on Simulations","ref_index":53,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25995","citing_title":"The evolution of the galaxy gas-phase mass-metallicity relation from $z=15$ to $z=0$ in the COLIBRE cosmological simulations","ref_index":84,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO","json":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO.json","graph_json":"https://pith.science/api/pith-number/RPHDKHDACOZFWX53TKSNGQWFDO/graph.json","events_json":"https://pith.science/api/pith-number/RPHDKHDACOZFWX53TKSNGQWFDO/events.json","paper":"https://pith.science/paper/RPHDKHDA"},"agent_actions":{"view_html":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO","download_json":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO.json","view_paper":"https://pith.science/paper/RPHDKHDA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0605120&json=true","fetch_graph":"https://pith.science/api/pith-number/RPHDKHDACOZFWX53TKSNGQWFDO/graph.json","fetch_events":"https://pith.science/api/pith-number/RPHDKHDACOZFWX53TKSNGQWFDO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO/action/storage_attestation","attest_author":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO/action/author_attestation","sign_citation":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO/action/citation_signature","submit_replication":"https://pith.science/pith/RPHDKHDACOZFWX53TKSNGQWFDO/action/replication_record"}},"created_at":"2026-07-04T15:22:18.935444+00:00","updated_at":"2026-07-04T15:22:18.935444+00:00"}