{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:CSXIGDAASDOMU74H7VOJ2MG5B2","short_pith_number":"pith:CSXIGDAA","schema_version":"1.0","canonical_sha256":"14ae830c0090dcca7f87fd5c9d30dd0e9d78efa392508ba63b08ad4da8287034","source":{"kind":"arxiv","id":"1707.02295","version":1},"attestation_state":"computed","paper":{"title":"Solar plasma radio emission in the presence of imbalanced turbulence of kinetic-scale Alfv\\'en waves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.SR","physics.plasm-ph"],"primary_cat":"physics.space-ph","authors_text":"Donald Melrose, Eduard Kontar, Nicolas Bian, Olena Lyubchyk, Yuriy Voitenko","submitted_at":"2017-07-07T13:10:53Z","abstract_excerpt":"We study the influence of kinetic-scale Alfv\\'enic turbulence on the generation of plasma radio emission in the solar coronal regions where the plasma/magnetic pressure ratio $\\beta $ is smaller than the electron/ion mass ratio $m_{e}/m_{i}$. The present study is motivated by the phenomenon of solar type I radio storms associated with the strong magnetic field of active regions. The measured brightness temperature of the type I storms can be up to $10^{10}$ K for continuum emission, and can exceed $10^{11}$ K for type I bursts. At present, there is no generally accepted theory explaining such "},"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":"1707.02295","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"physics.space-ph","submitted_at":"2017-07-07T13:10:53Z","cross_cats_sorted":["astro-ph.HE","astro-ph.SR","physics.plasm-ph"],"title_canon_sha256":"ff02412bc1a7d192de97a2da4bd9814b0ac3d5e7a19d7d482a904885c33ab183","abstract_canon_sha256":"ae0b7abb9edaae5d15527d007c0657b4e887665a2bcd09f254959923e695ed5b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:31:30.989748Z","signature_b64":"+WIIAMsOXZBfEUujaduDN67kAOKH0HiRR5e2qp2YL1+piT5McftLmFvEe1rH3ZpbOeM2rMgnATlQepS6vShBDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"14ae830c0090dcca7f87fd5c9d30dd0e9d78efa392508ba63b08ad4da8287034","last_reissued_at":"2026-05-18T00:31:30.988272Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:31:30.988272Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Solar plasma radio emission in the presence of imbalanced turbulence of kinetic-scale Alfv\\'en waves","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.SR","physics.plasm-ph"],"primary_cat":"physics.space-ph","authors_text":"Donald Melrose, Eduard Kontar, Nicolas Bian, Olena Lyubchyk, Yuriy Voitenko","submitted_at":"2017-07-07T13:10:53Z","abstract_excerpt":"We study the influence of kinetic-scale Alfv\\'enic turbulence on the generation of plasma radio emission in the solar coronal regions where the plasma/magnetic pressure ratio $\\beta $ is smaller than the electron/ion mass ratio $m_{e}/m_{i}$. The present study is motivated by the phenomenon of solar type I radio storms associated with the strong magnetic field of active regions. The measured brightness temperature of the type I storms can be up to $10^{10}$ K for continuum emission, and can exceed $10^{11}$ K for type I bursts. At present, there is no generally accepted theory explaining such "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1707.02295","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":""},"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":"1707.02295","created_at":"2026-05-18T00:31:30.988969+00:00"},{"alias_kind":"arxiv_version","alias_value":"1707.02295v1","created_at":"2026-05-18T00:31:30.988969+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1707.02295","created_at":"2026-05-18T00:31:30.988969+00:00"},{"alias_kind":"pith_short_12","alias_value":"CSXIGDAASDOM","created_at":"2026-05-18T12:31:10.602751+00:00"},{"alias_kind":"pith_short_16","alias_value":"CSXIGDAASDOMU74H","created_at":"2026-05-18T12:31:10.602751+00:00"},{"alias_kind":"pith_short_8","alias_value":"CSXIGDAA","created_at":"2026-05-18T12:31:10.602751+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2","json":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2.json","graph_json":"https://pith.science/api/pith-number/CSXIGDAASDOMU74H7VOJ2MG5B2/graph.json","events_json":"https://pith.science/api/pith-number/CSXIGDAASDOMU74H7VOJ2MG5B2/events.json","paper":"https://pith.science/paper/CSXIGDAA"},"agent_actions":{"view_html":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2","download_json":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2.json","view_paper":"https://pith.science/paper/CSXIGDAA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1707.02295&json=true","fetch_graph":"https://pith.science/api/pith-number/CSXIGDAASDOMU74H7VOJ2MG5B2/graph.json","fetch_events":"https://pith.science/api/pith-number/CSXIGDAASDOMU74H7VOJ2MG5B2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2/action/storage_attestation","attest_author":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2/action/author_attestation","sign_citation":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2/action/citation_signature","submit_replication":"https://pith.science/pith/CSXIGDAASDOMU74H7VOJ2MG5B2/action/replication_record"}},"created_at":"2026-05-18T00:31:30.988969+00:00","updated_at":"2026-05-18T00:31:30.988969+00:00"}