{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:PVV6V3J5YDOQVTARZCRF52RCW5","short_pith_number":"pith:PVV6V3J5","schema_version":"1.0","canonical_sha256":"7d6beaed3dc0dd0acc11c8a25eea22b76a32650a599d893de9dfa2ac01226e0d","source":{"kind":"arxiv","id":"2104.13093","version":2},"attestation_state":"computed","paper":{"title":"Regimes of cosmic-ray diffusion in Galactic turbulence","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"E.G. Zweibel, J. Becker Tjus, J. D\\\"orner, L. Merten, M.J. Pueschel, P. Reichherzer","submitted_at":"2021-04-27T10:30:03Z","abstract_excerpt":"Cosmic-ray transport in astrophysical environments is often dominated by the diffusion of particles in a magnetic field composed of both a turbulent and a mean component. This process, which is two-fold turbulent mixing in that the particle motion is stochastic with respect to the field lines, needs to be understood in order to properly model cosmic-ray signatures. One of the most important aspects in the modeling of cosmic-ray diffusion is that fully resonant scattering, the most effective such process, is only possible if the wave spectrum covers the entire range of propagation angles. By ta"},"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":"2104.13093","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-04-27T10:30:03Z","cross_cats_sorted":[],"title_canon_sha256":"3b27d3b845ad94de3204c9b830b2e9016d0c06a5337bb2f37e0a3c6e6affe70a","abstract_canon_sha256":"bc93260a4aaef64c5f1cefa65630d957f9d2d9082dcb0eddfb771558680f942c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:39:58.744397Z","signature_b64":"gTHdpx0tZo4EGIunSXeSn9JifdlBz3WtTDFj6KfzrrzArwO5jmfDtZw5nnGnajsOqmpIn+6TjpeaBTOhl5FkCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7d6beaed3dc0dd0acc11c8a25eea22b76a32650a599d893de9dfa2ac01226e0d","last_reissued_at":"2026-07-05T03:39:58.743872Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:39:58.743872Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Regimes of cosmic-ray diffusion in Galactic turbulence","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"E.G. Zweibel, J. Becker Tjus, J. D\\\"orner, L. Merten, M.J. Pueschel, P. Reichherzer","submitted_at":"2021-04-27T10:30:03Z","abstract_excerpt":"Cosmic-ray transport in astrophysical environments is often dominated by the diffusion of particles in a magnetic field composed of both a turbulent and a mean component. This process, which is two-fold turbulent mixing in that the particle motion is stochastic with respect to the field lines, needs to be understood in order to properly model cosmic-ray signatures. One of the most important aspects in the modeling of cosmic-ray diffusion is that fully resonant scattering, the most effective such process, is only possible if the wave spectrum covers the entire range of propagation angles. By ta"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2104.13093","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/2104.13093/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":"2104.13093","created_at":"2026-07-05T03:39:58.743933+00:00"},{"alias_kind":"arxiv_version","alias_value":"2104.13093v2","created_at":"2026-07-05T03:39:58.743933+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2104.13093","created_at":"2026-07-05T03:39:58.743933+00:00"},{"alias_kind":"pith_short_12","alias_value":"PVV6V3J5YDOQ","created_at":"2026-07-05T03:39:58.743933+00:00"},{"alias_kind":"pith_short_16","alias_value":"PVV6V3J5YDOQVTAR","created_at":"2026-07-05T03:39:58.743933+00:00"},{"alias_kind":"pith_short_8","alias_value":"PVV6V3J5","created_at":"2026-07-05T03:39:58.743933+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2310.16594","citing_title":"Constraining the slow-diffusion zone size and electron injection spectral index for the Geminga pulsar halo","ref_index":43,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5","json":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5.json","graph_json":"https://pith.science/api/pith-number/PVV6V3J5YDOQVTARZCRF52RCW5/graph.json","events_json":"https://pith.science/api/pith-number/PVV6V3J5YDOQVTARZCRF52RCW5/events.json","paper":"https://pith.science/paper/PVV6V3J5"},"agent_actions":{"view_html":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5","download_json":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5.json","view_paper":"https://pith.science/paper/PVV6V3J5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2104.13093&json=true","fetch_graph":"https://pith.science/api/pith-number/PVV6V3J5YDOQVTARZCRF52RCW5/graph.json","fetch_events":"https://pith.science/api/pith-number/PVV6V3J5YDOQVTARZCRF52RCW5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5/action/storage_attestation","attest_author":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5/action/author_attestation","sign_citation":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5/action/citation_signature","submit_replication":"https://pith.science/pith/PVV6V3J5YDOQVTARZCRF52RCW5/action/replication_record"}},"created_at":"2026-07-05T03:39:58.743933+00:00","updated_at":"2026-07-05T03:39:58.743933+00:00"}