{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:7TCRQVOXWGTYYTNBHKKHJJLBF3","short_pith_number":"pith:7TCRQVOX","schema_version":"1.0","canonical_sha256":"fcc51855d7b1a78c4da13a9474a5612ef1ecffc7d36f40d02b3df8efd44e6e53","source":{"kind":"arxiv","id":"2205.08174","version":2},"attestation_state":"computed","paper":{"title":"Turbulent diffusion of streaming cosmic rays in compressible, partially ionised plasma","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Amit Seta, Christoph Federrath, James R. Beattie, Mark R. Krumholz, Matt L. Sampson, Roland M. Crocker","submitted_at":"2022-05-17T08:26:16Z","abstract_excerpt":"Cosmic rays (CRs) are a dynamically important component of the interstellar medium (ISM) of galaxies. The $\\sim$GeV CRs that carry most CR energy and pressure are likely confined by self-generated turbulence, leading them to stream along magnetic field lines at the ion Alfv\\'en speed. However, the consequences of self-confinement for CR propagation on galaxy scales remain highly uncertain. In this paper, we use a large ensemble of magnetohydrodynamical turbulence simulations to quantify how the basic parameters describing ISM turbulence -- the sonic Mach number, $\\mathcal{M}$ (plasma compressi"},"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":"2205.08174","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2022-05-17T08:26:16Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"a2cc3d05b9d2d650ec34eb0f9fa640478996c04c756bcda3cc4e11cc94e86742","abstract_canon_sha256":"f5810f10e298eb84b99d8054924632cdbcd0fb386d58f00c8d93ee42c89ddf3b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:16:18.753687Z","signature_b64":"nteGGzi1K5FwfhyQNCeX6mhEjsceoS+3wCYozvjZvvSHZjsa4j7w5gd8Oy/wSf2VrsJr98EQBRclvxo0bsxtCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fcc51855d7b1a78c4da13a9474a5612ef1ecffc7d36f40d02b3df8efd44e6e53","last_reissued_at":"2026-07-05T05:16:18.753096Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:16:18.753096Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Turbulent diffusion of streaming cosmic rays in compressible, partially ionised plasma","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Amit Seta, Christoph Federrath, James R. Beattie, Mark R. Krumholz, Matt L. Sampson, Roland M. Crocker","submitted_at":"2022-05-17T08:26:16Z","abstract_excerpt":"Cosmic rays (CRs) are a dynamically important component of the interstellar medium (ISM) of galaxies. The $\\sim$GeV CRs that carry most CR energy and pressure are likely confined by self-generated turbulence, leading them to stream along magnetic field lines at the ion Alfv\\'en speed. However, the consequences of self-confinement for CR propagation on galaxy scales remain highly uncertain. In this paper, we use a large ensemble of magnetohydrodynamical turbulence simulations to quantify how the basic parameters describing ISM turbulence -- the sonic Mach number, $\\mathcal{M}$ (plasma compressi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2205.08174","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/2205.08174/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":"2205.08174","created_at":"2026-07-05T05:16:18.753184+00:00"},{"alias_kind":"arxiv_version","alias_value":"2205.08174v2","created_at":"2026-07-05T05:16:18.753184+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2205.08174","created_at":"2026-07-05T05:16:18.753184+00:00"},{"alias_kind":"pith_short_12","alias_value":"7TCRQVOXWGTY","created_at":"2026-07-05T05:16:18.753184+00:00"},{"alias_kind":"pith_short_16","alias_value":"7TCRQVOXWGTYYTNB","created_at":"2026-07-05T05:16:18.753184+00:00"},{"alias_kind":"pith_short_8","alias_value":"7TCRQVOX","created_at":"2026-07-05T05:16:18.753184+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.07741","citing_title":"Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to H$\\alpha$ Surface Brightness Ratio","ref_index":279,"is_internal_anchor":false},{"citing_arxiv_id":"2604.11898","citing_title":"Beyond the Diffusion Coefficient: Propagators and Memory in Cosmic Ray Transport","ref_index":44,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3","json":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3.json","graph_json":"https://pith.science/api/pith-number/7TCRQVOXWGTYYTNBHKKHJJLBF3/graph.json","events_json":"https://pith.science/api/pith-number/7TCRQVOXWGTYYTNBHKKHJJLBF3/events.json","paper":"https://pith.science/paper/7TCRQVOX"},"agent_actions":{"view_html":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3","download_json":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3.json","view_paper":"https://pith.science/paper/7TCRQVOX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2205.08174&json=true","fetch_graph":"https://pith.science/api/pith-number/7TCRQVOXWGTYYTNBHKKHJJLBF3/graph.json","fetch_events":"https://pith.science/api/pith-number/7TCRQVOXWGTYYTNBHKKHJJLBF3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3/action/storage_attestation","attest_author":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3/action/author_attestation","sign_citation":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3/action/citation_signature","submit_replication":"https://pith.science/pith/7TCRQVOXWGTYYTNBHKKHJJLBF3/action/replication_record"}},"created_at":"2026-07-05T05:16:18.753184+00:00","updated_at":"2026-07-05T05:16:18.753184+00:00"}