{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:55GCD73OWLN3277CHHMDHN4VY2","short_pith_number":"pith:55GCD73O","schema_version":"1.0","canonical_sha256":"ef4c21ff6eb2dbbd7fe239d833b795c6a1a3fb5312cd81bed4e3687156b58dea","source":{"kind":"arxiv","id":"2506.16816","version":1},"attestation_state":"computed","paper":{"title":"Electromagnetic radiation by turbulent, magnetized and randomly inhomogeneous solar radio sources generated by electron beams","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.SR","authors_text":"Alexandr Volokitin, Catherine Krafft, Francisco Javier Polanco-Rodr\\'iguez, Philippe Savoini","submitted_at":"2025-06-20T08:11:10Z","abstract_excerpt":"During Type III solar radio bursts, electromagnetic waves are radiated at plasma frequency $\\omega_p$ and its harmonics by electrostatic wave turbulence generated by electron beams ejected by Sun in randomly inhomogeneous solar wind and coronal plasmas. These emissions, detected since decades by spacecraft and radiotelescopes, are split by the plasma magnetic field into three modes $\\mathcal{X}$, $\\mathcal{O}$ and $\\mathcal{Z}$ of different dispersion, polarization and radiation properties. This work demonstrates, using three independent and converging approaches, that only a small fraction of"},"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":"2506.16816","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.SR","submitted_at":"2025-06-20T08:11:10Z","cross_cats_sorted":["physics.plasm-ph"],"title_canon_sha256":"bb89d71f508aaf0d38b46a024cc9345b334997c7ee951b729e0bba476cf327a5","abstract_canon_sha256":"645e0534da958d55e82cf08c08f81c1d1981e9a5bcad61429747433cdd9f7710"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:51:30.679612Z","signature_b64":"rUs6My2WnS0UsSbkttIg7xwl5TV0f4Dom7ZRCqaTPkedBD89PTC8hK1m28lt8BfTqylqqL/c2ihunNrUb3w/Bw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ef4c21ff6eb2dbbd7fe239d833b795c6a1a3fb5312cd81bed4e3687156b58dea","last_reissued_at":"2026-07-05T11:51:30.679122Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:51:30.679122Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Electromagnetic radiation by turbulent, magnetized and randomly inhomogeneous solar radio sources generated by electron beams","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["physics.plasm-ph"],"primary_cat":"astro-ph.SR","authors_text":"Alexandr Volokitin, Catherine Krafft, Francisco Javier Polanco-Rodr\\'iguez, Philippe Savoini","submitted_at":"2025-06-20T08:11:10Z","abstract_excerpt":"During Type III solar radio bursts, electromagnetic waves are radiated at plasma frequency $\\omega_p$ and its harmonics by electrostatic wave turbulence generated by electron beams ejected by Sun in randomly inhomogeneous solar wind and coronal plasmas. These emissions, detected since decades by spacecraft and radiotelescopes, are split by the plasma magnetic field into three modes $\\mathcal{X}$, $\\mathcal{O}$ and $\\mathcal{Z}$ of different dispersion, polarization and radiation properties. This work demonstrates, using three independent and converging approaches, that only a small fraction of"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2506.16816","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/2506.16816/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":"2506.16816","created_at":"2026-07-05T11:51:30.679177+00:00"},{"alias_kind":"arxiv_version","alias_value":"2506.16816v1","created_at":"2026-07-05T11:51:30.679177+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2506.16816","created_at":"2026-07-05T11:51:30.679177+00:00"},{"alias_kind":"pith_short_12","alias_value":"55GCD73OWLN3","created_at":"2026-07-05T11:51:30.679177+00:00"},{"alias_kind":"pith_short_16","alias_value":"55GCD73OWLN3277C","created_at":"2026-07-05T11:51:30.679177+00:00"},{"alias_kind":"pith_short_8","alias_value":"55GCD73O","created_at":"2026-07-05T11:51:30.679177+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.13856","citing_title":"Linear mode conversion theory of radio emission from turbulent solar wind plasmas","ref_index":22,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2","json":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2.json","graph_json":"https://pith.science/api/pith-number/55GCD73OWLN3277CHHMDHN4VY2/graph.json","events_json":"https://pith.science/api/pith-number/55GCD73OWLN3277CHHMDHN4VY2/events.json","paper":"https://pith.science/paper/55GCD73O"},"agent_actions":{"view_html":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2","download_json":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2.json","view_paper":"https://pith.science/paper/55GCD73O","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2506.16816&json=true","fetch_graph":"https://pith.science/api/pith-number/55GCD73OWLN3277CHHMDHN4VY2/graph.json","fetch_events":"https://pith.science/api/pith-number/55GCD73OWLN3277CHHMDHN4VY2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2/action/storage_attestation","attest_author":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2/action/author_attestation","sign_citation":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2/action/citation_signature","submit_replication":"https://pith.science/pith/55GCD73OWLN3277CHHMDHN4VY2/action/replication_record"}},"created_at":"2026-07-05T11:51:30.679177+00:00","updated_at":"2026-07-05T11:51:30.679177+00:00"}