{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:YBBJ2HFKPGNLZSZK7FWUC7VCXK","short_pith_number":"pith:YBBJ2HFK","schema_version":"1.0","canonical_sha256":"c0429d1caa799abccb2af96d417ea2ba9e4584bc258724f5084e6b7124f7ee50","source":{"kind":"arxiv","id":"2402.16336","version":1},"attestation_state":"computed","paper":{"title":"Red Asymmetry of H$_{\\alpha}$ Line Profiles during the flares on the active RS CVn-type star II Pegasi","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Dongtao Cao, Shenghong Gu","submitted_at":"2024-02-26T06:33:10Z","abstract_excerpt":"Stellar coronal mass ejections (CMEs) have recently attracted much attention for their impacts on stellar evolution and surrounding exoplanets. RS CVn-type stars could produce large flares, and therefore may have frequent CMEs. Here we report the capture of a possible CME or chromospheric condensation on the RS CVn-type star II Pegasi (II Peg) using high-resolution spectroscopic observation. Two flares were detected during the observation, and the low limits of the flare energies are of the order of $10^{33}$ erg and $10^{34}$ erg, respectively. Using mean spectrum subtraction, the H$_{\\alpha}"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2402.16336","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2024-02-26T06:33:10Z","cross_cats_sorted":[],"title_canon_sha256":"3a12e8d09f15cd419a0c8b7935812c4c95938dc4f9d85e1a332b8d61034c10d1","abstract_canon_sha256":"c683fa188326382af512d6fba61441cf790408ff9235bb2cee491688585dbd7e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:49:20.448860Z","signature_b64":"yPw3ItrpkVmQieZzClnrLnBL5IgKHxmutQ5zyn191GKMH3o5qUvqwwA/4A4N8hHbLiGSBWgl7wO3u6KkqqCyBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c0429d1caa799abccb2af96d417ea2ba9e4584bc258724f5084e6b7124f7ee50","last_reissued_at":"2026-07-05T07:49:20.448421Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:49:20.448421Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Red Asymmetry of H$_{\\alpha}$ Line Profiles during the flares on the active RS CVn-type star II Pegasi","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Dongtao Cao, Shenghong Gu","submitted_at":"2024-02-26T06:33:10Z","abstract_excerpt":"Stellar coronal mass ejections (CMEs) have recently attracted much attention for their impacts on stellar evolution and surrounding exoplanets. RS CVn-type stars could produce large flares, and therefore may have frequent CMEs. Here we report the capture of a possible CME or chromospheric condensation on the RS CVn-type star II Pegasi (II Peg) using high-resolution spectroscopic observation. Two flares were detected during the observation, and the low limits of the flare energies are of the order of $10^{33}$ erg and $10^{34}$ erg, respectively. Using mean spectrum subtraction, the H$_{\\alpha}"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2402.16336","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/2402.16336/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":"2402.16336","created_at":"2026-07-05T07:49:20.448478+00:00"},{"alias_kind":"arxiv_version","alias_value":"2402.16336v1","created_at":"2026-07-05T07:49:20.448478+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2402.16336","created_at":"2026-07-05T07:49:20.448478+00:00"},{"alias_kind":"pith_short_12","alias_value":"YBBJ2HFKPGNL","created_at":"2026-07-05T07:49:20.448478+00:00"},{"alias_kind":"pith_short_16","alias_value":"YBBJ2HFKPGNLZSZK","created_at":"2026-07-05T07:49:20.448478+00:00"},{"alias_kind":"pith_short_8","alias_value":"YBBJ2HFK","created_at":"2026-07-05T07:49:20.448478+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.04196","citing_title":"Probing Flare-Associated Eruptions on AB Doradus via X-ray Absorption Variations","ref_index":25,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK","json":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK.json","graph_json":"https://pith.science/api/pith-number/YBBJ2HFKPGNLZSZK7FWUC7VCXK/graph.json","events_json":"https://pith.science/api/pith-number/YBBJ2HFKPGNLZSZK7FWUC7VCXK/events.json","paper":"https://pith.science/paper/YBBJ2HFK"},"agent_actions":{"view_html":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK","download_json":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK.json","view_paper":"https://pith.science/paper/YBBJ2HFK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2402.16336&json=true","fetch_graph":"https://pith.science/api/pith-number/YBBJ2HFKPGNLZSZK7FWUC7VCXK/graph.json","fetch_events":"https://pith.science/api/pith-number/YBBJ2HFKPGNLZSZK7FWUC7VCXK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK/action/storage_attestation","attest_author":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK/action/author_attestation","sign_citation":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK/action/citation_signature","submit_replication":"https://pith.science/pith/YBBJ2HFKPGNLZSZK7FWUC7VCXK/action/replication_record"}},"created_at":"2026-07-05T07:49:20.448478+00:00","updated_at":"2026-07-05T07:49:20.448478+00:00"}