{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:T3MATOHFA5FJEK5BZEWJMNH3WG","short_pith_number":"pith:T3MATOHF","schema_version":"1.0","canonical_sha256":"9ed809b8e5074a922ba1c92c9634fbb18414f013d1b7b24c2e39409f6ef5c54e","source":{"kind":"arxiv","id":"2304.01088","version":3},"attestation_state":"computed","paper":{"title":"The efficiency of electron acceleration during the impulsive phase of a solar flare","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","physics.space-ph"],"primary_cat":"astro-ph.SR","authors_text":"A. Gordon Emslie, Brian R. Dennis, Eduard P. Kontar, Galina G. Motorina","submitted_at":"2023-04-03T15:45:31Z","abstract_excerpt":"Solar flares are known to be prolific electron accelerators, yet identifying the mechanism(s) for such efficient electron acceleration in solar flare (and similar astrophysical settings) presents a major challenge. This is due in part to a lack of observational constraints related to conditions in the primary acceleration region itself. Accelerated electrons with energies above $\\sim$20~keV are revealed by hard X-ray (HXR) bremsstrahlung emission, while accelerated electrons with even higher energies manifest themselves through radio gyrosynchrotron emission. Here we show, for a well-observed "},"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":"2304.01088","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2023-04-03T15:45:31Z","cross_cats_sorted":["astro-ph.HE","physics.space-ph"],"title_canon_sha256":"6ca3c3b4548ea6be2f58d1ebab46e2f724d29efc0417b92abbed98aa0e371195","abstract_canon_sha256":"85b89b4d26c2296b76cc1dd1b8a32370a346e726209fd33c0590d840836b8236"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:01:18.456989Z","signature_b64":"1diuaDQA6sg8rgnhNGHH3nufyOCKN4rXd1kP5uh1H1FVZ+p/ZoQd8QdsAn7vDAtZaDPTpTB+1v/F7pW59bNUCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9ed809b8e5074a922ba1c92c9634fbb18414f013d1b7b24c2e39409f6ef5c54e","last_reissued_at":"2026-07-05T06:01:18.456497Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:01:18.456497Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The efficiency of electron acceleration during the impulsive phase of a solar flare","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","physics.space-ph"],"primary_cat":"astro-ph.SR","authors_text":"A. Gordon Emslie, Brian R. Dennis, Eduard P. Kontar, Galina G. Motorina","submitted_at":"2023-04-03T15:45:31Z","abstract_excerpt":"Solar flares are known to be prolific electron accelerators, yet identifying the mechanism(s) for such efficient electron acceleration in solar flare (and similar astrophysical settings) presents a major challenge. This is due in part to a lack of observational constraints related to conditions in the primary acceleration region itself. Accelerated electrons with energies above $\\sim$20~keV are revealed by hard X-ray (HXR) bremsstrahlung emission, while accelerated electrons with even higher energies manifest themselves through radio gyrosynchrotron emission. Here we show, for a well-observed "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2304.01088","kind":"arxiv","version":3},"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/2304.01088/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":"2304.01088","created_at":"2026-07-05T06:01:18.456555+00:00"},{"alias_kind":"arxiv_version","alias_value":"2304.01088v3","created_at":"2026-07-05T06:01:18.456555+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2304.01088","created_at":"2026-07-05T06:01:18.456555+00:00"},{"alias_kind":"pith_short_12","alias_value":"T3MATOHFA5FJ","created_at":"2026-07-05T06:01:18.456555+00:00"},{"alias_kind":"pith_short_16","alias_value":"T3MATOHFA5FJEK5B","created_at":"2026-07-05T06:01:18.456555+00:00"},{"alias_kind":"pith_short_8","alias_value":"T3MATOHF","created_at":"2026-07-05T06:01:18.456555+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2502.04769","citing_title":"Solar flares as electron accelerators: toward a resolution of the acceleration efficiency issue","ref_index":6,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG","json":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG.json","graph_json":"https://pith.science/api/pith-number/T3MATOHFA5FJEK5BZEWJMNH3WG/graph.json","events_json":"https://pith.science/api/pith-number/T3MATOHFA5FJEK5BZEWJMNH3WG/events.json","paper":"https://pith.science/paper/T3MATOHF"},"agent_actions":{"view_html":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG","download_json":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG.json","view_paper":"https://pith.science/paper/T3MATOHF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2304.01088&json=true","fetch_graph":"https://pith.science/api/pith-number/T3MATOHFA5FJEK5BZEWJMNH3WG/graph.json","fetch_events":"https://pith.science/api/pith-number/T3MATOHFA5FJEK5BZEWJMNH3WG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG/action/storage_attestation","attest_author":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG/action/author_attestation","sign_citation":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG/action/citation_signature","submit_replication":"https://pith.science/pith/T3MATOHFA5FJEK5BZEWJMNH3WG/action/replication_record"}},"created_at":"2026-07-05T06:01:18.456555+00:00","updated_at":"2026-07-05T06:01:18.456555+00:00"}