{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:SFOODROJSP6P2LYUMCX52K4HS4","short_pith_number":"pith:SFOODROJ","schema_version":"1.0","canonical_sha256":"915ce1c5c993fcfd2f1460afdd2b879735ed8eb143480746344387041b241173","source":{"kind":"arxiv","id":"1809.09101","version":2},"attestation_state":"computed","paper":{"title":"Simulations of radiative turbulent mixing layers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Phillip Masterson, S. Peng Oh, Suoqing Ji","submitted_at":"2018-09-24T18:00:00Z","abstract_excerpt":"Radiative turbulent mixing layers should be ubiquitous in multi-phase gas with shear flow. They are a potentially attractive explanation for the high ions such as OVI seen in high velocity clouds and the circumgalactic medium (CGM) of galaxies. We perform 3D MHD simulations with non-equilibrium (NEI) and photoionization modeling, with an eye towards testing simple analytic models. Even purely hydrodynamic collisional ionization equilibrium (CIE) calculations have column densities much lower than observations. Characteristic inflow and turbulent velocities are much less than the shear velocity,"},"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":"1809.09101","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2018-09-24T18:00:00Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"d460b9d8c308d324c83e43614333c0a2fcb7770b30b56463dea1d50415666003","abstract_canon_sha256":"3b421a0d7f5c96ea7d325e4ef9dbe5d6d4eaf48900e78b0a11354a7b6a7881a1"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:46:03.960182Z","signature_b64":"/ZwNROnqpR7AEka9rerXg2yYWH+Slfq/PkusTQxAkU9ZymfS3o2FvEuGXSqWxxyGaEfx8tHBCguN+dQ5iVJxCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"915ce1c5c993fcfd2f1460afdd2b879735ed8eb143480746344387041b241173","last_reissued_at":"2026-05-17T23:46:03.959609Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:46:03.959609Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulations of radiative turbulent mixing layers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Phillip Masterson, S. Peng Oh, Suoqing Ji","submitted_at":"2018-09-24T18:00:00Z","abstract_excerpt":"Radiative turbulent mixing layers should be ubiquitous in multi-phase gas with shear flow. They are a potentially attractive explanation for the high ions such as OVI seen in high velocity clouds and the circumgalactic medium (CGM) of galaxies. We perform 3D MHD simulations with non-equilibrium (NEI) and photoionization modeling, with an eye towards testing simple analytic models. Even purely hydrodynamic collisional ionization equilibrium (CIE) calculations have column densities much lower than observations. Characteristic inflow and turbulent velocities are much less than the shear velocity,"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1809.09101","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":"1809.09101","created_at":"2026-05-17T23:46:03.959696+00:00"},{"alias_kind":"arxiv_version","alias_value":"1809.09101v2","created_at":"2026-05-17T23:46:03.959696+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1809.09101","created_at":"2026-05-17T23:46:03.959696+00:00"},{"alias_kind":"pith_short_12","alias_value":"SFOODROJSP6P","created_at":"2026-05-18T12:32:53.628368+00:00"},{"alias_kind":"pith_short_16","alias_value":"SFOODROJSP6P2LYU","created_at":"2026-05-18T12:32:53.628368+00:00"},{"alias_kind":"pith_short_8","alias_value":"SFOODROJ","created_at":"2026-05-18T12:32:53.628368+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.15275","citing_title":"The Simulated Oxygen Shortage (SOS): Mapping the Missing OVI in Simulated Dwarf Galaxies to Subgrid Physics","ref_index":64,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4","json":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4.json","graph_json":"https://pith.science/api/pith-number/SFOODROJSP6P2LYUMCX52K4HS4/graph.json","events_json":"https://pith.science/api/pith-number/SFOODROJSP6P2LYUMCX52K4HS4/events.json","paper":"https://pith.science/paper/SFOODROJ"},"agent_actions":{"view_html":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4","download_json":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4.json","view_paper":"https://pith.science/paper/SFOODROJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1809.09101&json=true","fetch_graph":"https://pith.science/api/pith-number/SFOODROJSP6P2LYUMCX52K4HS4/graph.json","fetch_events":"https://pith.science/api/pith-number/SFOODROJSP6P2LYUMCX52K4HS4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4/action/storage_attestation","attest_author":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4/action/author_attestation","sign_citation":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4/action/citation_signature","submit_replication":"https://pith.science/pith/SFOODROJSP6P2LYUMCX52K4HS4/action/replication_record"}},"created_at":"2026-05-17T23:46:03.959696+00:00","updated_at":"2026-05-17T23:46:03.959696+00:00"}