{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:A7C4RZI27DF6V7VPZ3NIXKBMOX","short_pith_number":"pith:A7C4RZI2","schema_version":"1.0","canonical_sha256":"07c5c8e51af8cbeafeafceda8ba82c75c743fa920a8a1e51fa4595d16c032809","source":{"kind":"arxiv","id":"1702.07338","version":3},"attestation_state":"computed","paper":{"title":"Investigating the Magnetic Imprints of Major Solar Eruptions with SDO/HMI High-Cadence Vector Magnetograms","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"J. Todd Hoeksema, Maria Kazachenko, Ruizhu Chen, Xudong Sun, Yang Liu","submitted_at":"2017-02-23T18:51:58Z","abstract_excerpt":"The solar active region photospheric magnetic field evolves rapidly during major eruptive events, suggesting appreciable feedback from the corona. Previous studies of these \"magnetic imprints\" are mostly based on line-of-sight only or lower-cadence vector observations; a temporally resolved depiction of the vector field evolution is hitherto lacking. Here, we introduce the high-cadence (90~s or 135~s) vector magnetogram dataset from the Helioseismic and Magnetic Imager (HMI) that is well suited for investigating the phenomenon. These observations allow quantitative characterization of the perm"},"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":"1702.07338","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2017-02-23T18:51:58Z","cross_cats_sorted":[],"title_canon_sha256":"19f43ee1fb37655d19f904c74413f6e1fe56312711fef3ecaeda660b508de496","abstract_canon_sha256":"4d9758d8b4c9a69a5414a1473b69389c7c920aea732f9fe9a1cd62a49d9f8fe6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:45:41.943620Z","signature_b64":"IMwKCkNdMxKtDwbiaIQF6/y3SpOPD6n6xv9/S56qAV3JAfv6Dj5nCWCVySGQ8SzVTO0O022euHBuJi1LtORoAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"07c5c8e51af8cbeafeafceda8ba82c75c743fa920a8a1e51fa4595d16c032809","last_reissued_at":"2026-05-18T00:45:41.943089Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:45:41.943089Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Investigating the Magnetic Imprints of Major Solar Eruptions with SDO/HMI High-Cadence Vector Magnetograms","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"J. Todd Hoeksema, Maria Kazachenko, Ruizhu Chen, Xudong Sun, Yang Liu","submitted_at":"2017-02-23T18:51:58Z","abstract_excerpt":"The solar active region photospheric magnetic field evolves rapidly during major eruptive events, suggesting appreciable feedback from the corona. Previous studies of these \"magnetic imprints\" are mostly based on line-of-sight only or lower-cadence vector observations; a temporally resolved depiction of the vector field evolution is hitherto lacking. Here, we introduce the high-cadence (90~s or 135~s) vector magnetogram dataset from the Helioseismic and Magnetic Imager (HMI) that is well suited for investigating the phenomenon. These observations allow quantitative characterization of the perm"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1702.07338","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":""},"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":"1702.07338","created_at":"2026-05-18T00:45:41.943165+00:00"},{"alias_kind":"arxiv_version","alias_value":"1702.07338v3","created_at":"2026-05-18T00:45:41.943165+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1702.07338","created_at":"2026-05-18T00:45:41.943165+00:00"},{"alias_kind":"pith_short_12","alias_value":"A7C4RZI27DF6","created_at":"2026-05-18T12:31:05.417338+00:00"},{"alias_kind":"pith_short_16","alias_value":"A7C4RZI27DF6V7VP","created_at":"2026-05-18T12:31:05.417338+00:00"},{"alias_kind":"pith_short_8","alias_value":"A7C4RZI2","created_at":"2026-05-18T12:31:05.417338+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.17195","citing_title":"On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfv\\'enic Supra-Arcade Plasma Downflows","ref_index":28,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX","json":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX.json","graph_json":"https://pith.science/api/pith-number/A7C4RZI27DF6V7VPZ3NIXKBMOX/graph.json","events_json":"https://pith.science/api/pith-number/A7C4RZI27DF6V7VPZ3NIXKBMOX/events.json","paper":"https://pith.science/paper/A7C4RZI2"},"agent_actions":{"view_html":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX","download_json":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX.json","view_paper":"https://pith.science/paper/A7C4RZI2","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1702.07338&json=true","fetch_graph":"https://pith.science/api/pith-number/A7C4RZI27DF6V7VPZ3NIXKBMOX/graph.json","fetch_events":"https://pith.science/api/pith-number/A7C4RZI27DF6V7VPZ3NIXKBMOX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX/action/storage_attestation","attest_author":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX/action/author_attestation","sign_citation":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX/action/citation_signature","submit_replication":"https://pith.science/pith/A7C4RZI27DF6V7VPZ3NIXKBMOX/action/replication_record"}},"created_at":"2026-05-18T00:45:41.943165+00:00","updated_at":"2026-05-18T00:45:41.943165+00:00"}