{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:QTG2B2L5TXN2RFSWBN25GIBP4J","short_pith_number":"pith:QTG2B2L5","schema_version":"1.0","canonical_sha256":"84cda0e97d9ddba896560b75d3202fe27af6e82f02d113ad708916b1259fcab3","source":{"kind":"arxiv","id":"1803.05436","version":1},"attestation_state":"computed","paper":{"title":"Evidence for a New Component of High-Energy Solar Gamma-Ray Production","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Annika H. G. Peter, Bei Zhou, John F. Beacom, Kenny C. Y. Ng, Qing-Wen Tang, Tim Linden","submitted_at":"2018-03-14T18:00:00Z","abstract_excerpt":"The observed multi-GeV gamma-ray emission from the solar disk --- sourced by hadronic cosmic rays interacting with gas, and affected by complex magnetic fields --- is not understood. Utilizing an improved analysis of the Fermi-LAT data that includes the first resolved imaging of the disk, we find strong evidence that this emission is produced by two separate mechanisms. Between 2010-2017 (the rise to and fall from solar maximum), the gamma-ray emission is dominated by a polar component. Between 2008-2009 (solar minimum) this component remains present, but the total emission is instead dominate"},"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":"1803.05436","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2018-03-14T18:00:00Z","cross_cats_sorted":["astro-ph.SR","hep-ph"],"title_canon_sha256":"838cb3c0f2048c230ce035197d58c12772ee86235326f08d19f5a937cf76f33b","abstract_canon_sha256":"4a4c0e408b3ee12d664a12170ac7a11e3ee3c6e74598481542364f94af85fd55"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:04:17.531368Z","signature_b64":"5d1C/kjC4hZMZselVH15dO79aoZI46i73v+Y/X/WQ0qVpumHxAFu6lQ57kDdYGmCuyPicA7EXdzKaN743butCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"84cda0e97d9ddba896560b75d3202fe27af6e82f02d113ad708916b1259fcab3","last_reissued_at":"2026-05-18T00:04:17.530674Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:04:17.530674Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Evidence for a New Component of High-Energy Solar Gamma-Ray Production","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR","hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Annika H. G. Peter, Bei Zhou, John F. Beacom, Kenny C. Y. Ng, Qing-Wen Tang, Tim Linden","submitted_at":"2018-03-14T18:00:00Z","abstract_excerpt":"The observed multi-GeV gamma-ray emission from the solar disk --- sourced by hadronic cosmic rays interacting with gas, and affected by complex magnetic fields --- is not understood. Utilizing an improved analysis of the Fermi-LAT data that includes the first resolved imaging of the disk, we find strong evidence that this emission is produced by two separate mechanisms. Between 2010-2017 (the rise to and fall from solar maximum), the gamma-ray emission is dominated by a polar component. Between 2008-2009 (solar minimum) this component remains present, but the total emission is instead dominate"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1803.05436","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":"1803.05436","created_at":"2026-05-18T00:04:17.530759+00:00"},{"alias_kind":"arxiv_version","alias_value":"1803.05436v1","created_at":"2026-05-18T00:04:17.530759+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1803.05436","created_at":"2026-05-18T00:04:17.530759+00:00"},{"alias_kind":"pith_short_12","alias_value":"QTG2B2L5TXN2","created_at":"2026-05-18T12:32:46.962924+00:00"},{"alias_kind":"pith_short_16","alias_value":"QTG2B2L5TXN2RFSW","created_at":"2026-05-18T12:32:46.962924+00:00"},{"alias_kind":"pith_short_8","alias_value":"QTG2B2L5","created_at":"2026-05-18T12:32:46.962924+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1907.07737","citing_title":"The Southern Wide-Field Gamma-Ray Observatory (SWGO): A Next-Generation Ground-Based Survey Instrument for VHE Gamma-Ray Astronomy","ref_index":57,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J","json":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J.json","graph_json":"https://pith.science/api/pith-number/QTG2B2L5TXN2RFSWBN25GIBP4J/graph.json","events_json":"https://pith.science/api/pith-number/QTG2B2L5TXN2RFSWBN25GIBP4J/events.json","paper":"https://pith.science/paper/QTG2B2L5"},"agent_actions":{"view_html":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J","download_json":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J.json","view_paper":"https://pith.science/paper/QTG2B2L5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1803.05436&json=true","fetch_graph":"https://pith.science/api/pith-number/QTG2B2L5TXN2RFSWBN25GIBP4J/graph.json","fetch_events":"https://pith.science/api/pith-number/QTG2B2L5TXN2RFSWBN25GIBP4J/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J/action/storage_attestation","attest_author":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J/action/author_attestation","sign_citation":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J/action/citation_signature","submit_replication":"https://pith.science/pith/QTG2B2L5TXN2RFSWBN25GIBP4J/action/replication_record"}},"created_at":"2026-05-18T00:04:17.530759+00:00","updated_at":"2026-05-18T00:04:17.530759+00:00"}