{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:U3JMUQQNAU5BJ7DRLUJRRXJ7XJ","short_pith_number":"pith:U3JMUQQN","schema_version":"1.0","canonical_sha256":"a6d2ca420d053a14fc715d1318dd3fba4517d7aa2103c7bf2e3b5f69961c0bde","source":{"kind":"arxiv","id":"2010.13825","version":2},"attestation_state":"computed","paper":{"title":"Novel interpretation of the latest AMS-02 cosmic-ray electron spectrum","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Fiorenza Donato, Mattia Di Mauro, Silvia Manconi","submitted_at":"2020-10-26T18:21:21Z","abstract_excerpt":"The latest AMS-02 data on cosmic ray electrons show a break in the energy spectrum around 40 GeV, with a change in the slope of about 0.1. We perform a combined fit to the newest AMS-02 positron and electron flux data above 10 GeV using a semi-analytical diffusion model where sources includes production of pairs from pulsar wind nebulae (PWNe), electrons from supernova remnants (SNRs) and both species from spallation of hadronic cosmic rays with interstellar medium atoms. We demonstrate that within our setup the change of slope in the AMS-02 electron data is well explained by the interplay bet"},"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":"2010.13825","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2020-10-26T18:21:21Z","cross_cats_sorted":[],"title_canon_sha256":"316150dc51fca70bb3ee6dfd854ec6d7ac755d395ae662c89521040c8e2bd54b","abstract_canon_sha256":"c404fcb41e4545dca69c1d18dd75f264de9636a2a5c636ff3d2d6a62a01ec791"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:26:37.731896Z","signature_b64":"mCNefLYUaoeP6c76PHvjTJ0HPoM0DSM70sUqIngJQC0pQ+ZlI/wMqxtpwPc4xulJZJpMA7xA+Ja3xVF8ZI1qBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a6d2ca420d053a14fc715d1318dd3fba4517d7aa2103c7bf2e3b5f69961c0bde","last_reissued_at":"2026-07-05T03:26:37.731379Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:26:37.731379Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Novel interpretation of the latest AMS-02 cosmic-ray electron spectrum","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Fiorenza Donato, Mattia Di Mauro, Silvia Manconi","submitted_at":"2020-10-26T18:21:21Z","abstract_excerpt":"The latest AMS-02 data on cosmic ray electrons show a break in the energy spectrum around 40 GeV, with a change in the slope of about 0.1. We perform a combined fit to the newest AMS-02 positron and electron flux data above 10 GeV using a semi-analytical diffusion model where sources includes production of pairs from pulsar wind nebulae (PWNe), electrons from supernova remnants (SNRs) and both species from spallation of hadronic cosmic rays with interstellar medium atoms. We demonstrate that within our setup the change of slope in the AMS-02 electron data is well explained by the interplay bet"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2010.13825","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/2010.13825/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":"2010.13825","created_at":"2026-07-05T03:26:37.731438+00:00"},{"alias_kind":"arxiv_version","alias_value":"2010.13825v2","created_at":"2026-07-05T03:26:37.731438+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2010.13825","created_at":"2026-07-05T03:26:37.731438+00:00"},{"alias_kind":"pith_short_12","alias_value":"U3JMUQQNAU5B","created_at":"2026-07-05T03:26:37.731438+00:00"},{"alias_kind":"pith_short_16","alias_value":"U3JMUQQNAU5BJ7DR","created_at":"2026-07-05T03:26:37.731438+00:00"},{"alias_kind":"pith_short_8","alias_value":"U3JMUQQN","created_at":"2026-07-05T03:26:37.731438+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.06011","citing_title":"SECRET: Stochasticity Emulator for Cosmic Ray Electrons","ref_index":13,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ","json":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ.json","graph_json":"https://pith.science/api/pith-number/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/graph.json","events_json":"https://pith.science/api/pith-number/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/events.json","paper":"https://pith.science/paper/U3JMUQQN"},"agent_actions":{"view_html":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ","download_json":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ.json","view_paper":"https://pith.science/paper/U3JMUQQN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2010.13825&json=true","fetch_graph":"https://pith.science/api/pith-number/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/graph.json","fetch_events":"https://pith.science/api/pith-number/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/action/storage_attestation","attest_author":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/action/author_attestation","sign_citation":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/action/citation_signature","submit_replication":"https://pith.science/pith/U3JMUQQNAU5BJ7DRLUJRRXJ7XJ/action/replication_record"}},"created_at":"2026-07-05T03:26:37.731438+00:00","updated_at":"2026-07-05T03:26:37.731438+00:00"}