{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:KTSBX2ETHBKKQCXTM3BTJ36YNQ","short_pith_number":"pith:KTSBX2ET","schema_version":"1.0","canonical_sha256":"54e41be8933854a80af366c334efd86c0e2859616a9847b0d23ac7e61033c3ce","source":{"kind":"arxiv","id":"2111.01143","version":1},"attestation_state":"computed","paper":{"title":"Self-Generated Cosmic-Ray Turbulence Can Explain the Morphology of TeV Halos","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Payel Mukhopadhyay, Tim Linden","submitted_at":"2021-11-01T18:00:01Z","abstract_excerpt":"Observations have shown that spatially extended \"TeV halos\" are a common (and potentially generic) feature surrounding young and middle-aged pulsars. However, their morphology is not understood. They are larger than the \"compact\" region where the stellar remnant dominates the properties of the interstellar medium, but smaller than expected in models of cosmic-ray diffusion through the standard interstellar medium. Several explanations have been proposed, but all have shortcomings. Here, we revisit a class of models where the cosmic-ray gradient produced by the central source induces a streamin"},"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":"2111.01143","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-11-01T18:00:01Z","cross_cats_sorted":["astro-ph.GA","hep-ph"],"title_canon_sha256":"641115ec6f28dab0726972dec6f8c5cbdf276fd3869b8018e2df9bf69208d306","abstract_canon_sha256":"ce6b7e711ba21c09297936e681e3257d8b5382d48adb8658537d8e51163f795c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:33:25.445431Z","signature_b64":"6OvMkjZD/5FI37cEUJQCAN5AABHPdVutqPWxI6OYydCbiUtWS/Sp9CRWnUeTGYYi4ZOb3bbFbtYCvBNG0zcYAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"54e41be8933854a80af366c334efd86c0e2859616a9847b0d23ac7e61033c3ce","last_reissued_at":"2026-07-05T04:33:25.444963Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:33:25.444963Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Self-Generated Cosmic-Ray Turbulence Can Explain the Morphology of TeV Halos","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Payel Mukhopadhyay, Tim Linden","submitted_at":"2021-11-01T18:00:01Z","abstract_excerpt":"Observations have shown that spatially extended \"TeV halos\" are a common (and potentially generic) feature surrounding young and middle-aged pulsars. However, their morphology is not understood. They are larger than the \"compact\" region where the stellar remnant dominates the properties of the interstellar medium, but smaller than expected in models of cosmic-ray diffusion through the standard interstellar medium. Several explanations have been proposed, but all have shortcomings. Here, we revisit a class of models where the cosmic-ray gradient produced by the central source induces a streamin"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2111.01143","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/2111.01143/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":"2111.01143","created_at":"2026-07-05T04:33:25.445018+00:00"},{"alias_kind":"arxiv_version","alias_value":"2111.01143v1","created_at":"2026-07-05T04:33:25.445018+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2111.01143","created_at":"2026-07-05T04:33:25.445018+00:00"},{"alias_kind":"pith_short_12","alias_value":"KTSBX2ETHBKK","created_at":"2026-07-05T04:33:25.445018+00:00"},{"alias_kind":"pith_short_16","alias_value":"KTSBX2ETHBKKQCXT","created_at":"2026-07-05T04:33:25.445018+00:00"},{"alias_kind":"pith_short_8","alias_value":"KTSBX2ET","created_at":"2026-07-05T04:33:25.445018+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"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":27,"is_internal_anchor":false},{"citing_arxiv_id":"2508.13667","citing_title":"PHECT: A lightweight computation tool for pulsar halo emission","ref_index":34,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ","json":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ.json","graph_json":"https://pith.science/api/pith-number/KTSBX2ETHBKKQCXTM3BTJ36YNQ/graph.json","events_json":"https://pith.science/api/pith-number/KTSBX2ETHBKKQCXTM3BTJ36YNQ/events.json","paper":"https://pith.science/paper/KTSBX2ET"},"agent_actions":{"view_html":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ","download_json":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ.json","view_paper":"https://pith.science/paper/KTSBX2ET","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2111.01143&json=true","fetch_graph":"https://pith.science/api/pith-number/KTSBX2ETHBKKQCXTM3BTJ36YNQ/graph.json","fetch_events":"https://pith.science/api/pith-number/KTSBX2ETHBKKQCXTM3BTJ36YNQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ/action/storage_attestation","attest_author":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ/action/author_attestation","sign_citation":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ/action/citation_signature","submit_replication":"https://pith.science/pith/KTSBX2ETHBKKQCXTM3BTJ36YNQ/action/replication_record"}},"created_at":"2026-07-05T04:33:25.445018+00:00","updated_at":"2026-07-05T04:33:25.445018+00:00"}