{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2001:B5BU5MTMMZGNZX2RGU73JXKSKA","short_pith_number":"pith:B5BU5MTM","schema_version":"1.0","canonical_sha256":"0f434eb26c664cdcdf51353fb4dd52501bdbd951dbdec6c343061b64d4d903b8","source":{"kind":"arxiv","id":"astro-ph/0101175","version":1},"attestation_state":"computed","paper":{"title":"Shock Acceleration of Cosmic Rays - a critical review","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) UKAEA Fusion, Culham), Heidelberg, J.G. Kirk (1), R.O. Dendy (2) ((1) Max-Planck-Institut fuer Kernphysik","submitted_at":"2001-01-11T09:51:04Z","abstract_excerpt":"Motivated by recent unsuccessful efforts to detect the predicted flux of TeV gamma-rays from supernova remnants, we present a critical examination of the theory on which these predictions are based. Three crucial problems are identified: injection, maximum achievable particle energy and spectral index. In each case significant new advances in understanding have been achieved, which cast doubt on prevailing paradigms such as Bohm diffusion and single-fluid MHD. This indicates that more realistic analytical models, backed by more sophisticated numerical techniques should be employed to obtain re"},"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/0101175","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2001-01-11T09:51:04Z","cross_cats_sorted":[],"title_canon_sha256":"133c5c1b94dbc24481668a23ffbf027dc2c888bd1a1a165a802b581092f2e7a4","abstract_canon_sha256":"b8adfddae55b272d1d940a06cd5c71d9d89f69fec900efaea976c90c8dfdcf2c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:20:39.118665Z","signature_b64":"NUYlaDJREqGQMsSQJx2vtSsaJVJx4xtmPRU85wjtg0pFkgLRP80ki6qMxZf6UH4Veluau8eCTHGHyIPAG4ffAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0f434eb26c664cdcdf51353fb4dd52501bdbd951dbdec6c343061b64d4d903b8","last_reissued_at":"2026-07-04T15:20:39.118245Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:20:39.118245Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Shock Acceleration of Cosmic Rays - a critical review","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) UKAEA Fusion, Culham), Heidelberg, J.G. Kirk (1), R.O. Dendy (2) ((1) Max-Planck-Institut fuer Kernphysik","submitted_at":"2001-01-11T09:51:04Z","abstract_excerpt":"Motivated by recent unsuccessful efforts to detect the predicted flux of TeV gamma-rays from supernova remnants, we present a critical examination of the theory on which these predictions are based. Three crucial problems are identified: injection, maximum achievable particle energy and spectral index. In each case significant new advances in understanding have been achieved, which cast doubt on prevailing paradigms such as Bohm diffusion and single-fluid MHD. This indicates that more realistic analytical models, backed by more sophisticated numerical techniques should be employed to obtain re"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0101175","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0101175/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/0101175","created_at":"2026-07-04T15:20:39.118306+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0101175v1","created_at":"2026-07-04T15:20:39.118306+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0101175","created_at":"2026-07-04T15:20:39.118306+00:00"},{"alias_kind":"pith_short_12","alias_value":"B5BU5MTMMZGN","created_at":"2026-07-04T15:20:39.118306+00:00"},{"alias_kind":"pith_short_16","alias_value":"B5BU5MTMMZGNZX2R","created_at":"2026-07-04T15:20:39.118306+00:00"},{"alias_kind":"pith_short_8","alias_value":"B5BU5MTM","created_at":"2026-07-04T15:20:39.118306+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.04212","citing_title":"Studying the mirror acceleration via kinetic simulations of relativistic plasma turbulence","ref_index":6,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA","json":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA.json","graph_json":"https://pith.science/api/pith-number/B5BU5MTMMZGNZX2RGU73JXKSKA/graph.json","events_json":"https://pith.science/api/pith-number/B5BU5MTMMZGNZX2RGU73JXKSKA/events.json","paper":"https://pith.science/paper/B5BU5MTM"},"agent_actions":{"view_html":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA","download_json":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA.json","view_paper":"https://pith.science/paper/B5BU5MTM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0101175&json=true","fetch_graph":"https://pith.science/api/pith-number/B5BU5MTMMZGNZX2RGU73JXKSKA/graph.json","fetch_events":"https://pith.science/api/pith-number/B5BU5MTMMZGNZX2RGU73JXKSKA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA/action/storage_attestation","attest_author":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA/action/author_attestation","sign_citation":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA/action/citation_signature","submit_replication":"https://pith.science/pith/B5BU5MTMMZGNZX2RGU73JXKSKA/action/replication_record"}},"created_at":"2026-07-04T15:20:39.118306+00:00","updated_at":"2026-07-04T15:20:39.118306+00:00"}