{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:OLUB2RUKCP3UOAJS4IBU4WE44I","short_pith_number":"pith:OLUB2RUK","schema_version":"1.0","canonical_sha256":"72e81d468a13f7470132e2034e589ce20a6ed81591386101133c8a0fcf72c4c8","source":{"kind":"arxiv","id":"1501.01377","version":1},"attestation_state":"computed","paper":{"title":"Spectroscopic variability of two Oe stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Fernando, A.F.J. Moffat, A. Hempelmann, Ba. Stober, Be. Stober, E.M. dos Santos, F. Alves, F. Marques Dias, G. Rauw, J.H. Knapen, J.H.M.M. Schmitt, J.N. Gonzalez-Perez, J. Ribeiro, J. Sanchez Gallego, K.-P. Schroeder, K. Vollmann, L.F. Gouveia Carreira, L. Schanne, M. Mittag, N.G. Correia Viegas, N. Reinecke, N. Romeo, O. Stahl, R. Fahed, R. Leadbeater, T. Bergmann, T. Eversberg, T. Hunger, T. Morel, W. Arnold, Y. Naze","submitted_at":"2015-01-07T07:16:40Z","abstract_excerpt":"The Oe stars HD45314 and HD60848 have recently been found to exhibit very different X-ray properties: whilst HD60848 has an X-ray spectrum and emission level typical of most OB stars, HD45314 features a much harder and brighter X-ray emission, making it a so-called gamma Cas analogue. Monitoring the optical spectra could provide hints towards the origin of these very different behaviours. We analyse a large set of spectroscopic observations of HD45314 and HD60848, extending over 20 years. We further attempt to fit the H-alpha line profiles of both stars with a simple model of emission line for"},"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":"1501.01377","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2015-01-07T07:16:40Z","cross_cats_sorted":[],"title_canon_sha256":"9621fa8b7a758a2d248af0eed6e40d2ba568d6eb3766c9d550a343810b4fe1a4","abstract_canon_sha256":"fc2c6f1194ca81aea62221ead3053564b72c86795d9c980390ab4003881f1a03"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:57:44.410331Z","signature_b64":"YMrpRVXFUoY+OJMx3cA/996J/kwyiRmy4k2sU47fTM8KYlpH0w0JcUa9AXqSkLaTFYGtNJyROZEwIGNhChQfBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"72e81d468a13f7470132e2034e589ce20a6ed81591386101133c8a0fcf72c4c8","last_reissued_at":"2026-07-05T01:57:44.409861Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:57:44.409861Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Spectroscopic variability of two Oe stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Fernando, A.F.J. Moffat, A. Hempelmann, Ba. Stober, Be. Stober, E.M. dos Santos, F. Alves, F. Marques Dias, G. Rauw, J.H. Knapen, J.H.M.M. Schmitt, J.N. Gonzalez-Perez, J. Ribeiro, J. Sanchez Gallego, K.-P. Schroeder, K. Vollmann, L.F. Gouveia Carreira, L. Schanne, M. Mittag, N.G. Correia Viegas, N. Reinecke, N. Romeo, O. Stahl, R. Fahed, R. Leadbeater, T. Bergmann, T. Eversberg, T. Hunger, T. Morel, W. Arnold, Y. Naze","submitted_at":"2015-01-07T07:16:40Z","abstract_excerpt":"The Oe stars HD45314 and HD60848 have recently been found to exhibit very different X-ray properties: whilst HD60848 has an X-ray spectrum and emission level typical of most OB stars, HD45314 features a much harder and brighter X-ray emission, making it a so-called gamma Cas analogue. Monitoring the optical spectra could provide hints towards the origin of these very different behaviours. We analyse a large set of spectroscopic observations of HD45314 and HD60848, extending over 20 years. We further attempt to fit the H-alpha line profiles of both stars with a simple model of emission line for"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1501.01377","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/1501.01377/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":"1501.01377","created_at":"2026-07-05T01:57:44.409931+00:00"},{"alias_kind":"arxiv_version","alias_value":"1501.01377v1","created_at":"2026-07-05T01:57:44.409931+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1501.01377","created_at":"2026-07-05T01:57:44.409931+00:00"},{"alias_kind":"pith_short_12","alias_value":"OLUB2RUKCP3U","created_at":"2026-07-05T01:57:44.409931+00:00"},{"alias_kind":"pith_short_16","alias_value":"OLUB2RUKCP3UOAJS","created_at":"2026-07-05T01:57:44.409931+00:00"},{"alias_kind":"pith_short_8","alias_value":"OLUB2RUK","created_at":"2026-07-05T01:57:44.409931+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/OLUB2RUKCP3UOAJS4IBU4WE44I","json":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I.json","graph_json":"https://pith.science/api/pith-number/OLUB2RUKCP3UOAJS4IBU4WE44I/graph.json","events_json":"https://pith.science/api/pith-number/OLUB2RUKCP3UOAJS4IBU4WE44I/events.json","paper":"https://pith.science/paper/OLUB2RUK"},"agent_actions":{"view_html":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I","download_json":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I.json","view_paper":"https://pith.science/paper/OLUB2RUK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1501.01377&json=true","fetch_graph":"https://pith.science/api/pith-number/OLUB2RUKCP3UOAJS4IBU4WE44I/graph.json","fetch_events":"https://pith.science/api/pith-number/OLUB2RUKCP3UOAJS4IBU4WE44I/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I/action/storage_attestation","attest_author":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I/action/author_attestation","sign_citation":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I/action/citation_signature","submit_replication":"https://pith.science/pith/OLUB2RUKCP3UOAJS4IBU4WE44I/action/replication_record"}},"created_at":"2026-07-05T01:57:44.409931+00:00","updated_at":"2026-07-05T01:57:44.409931+00:00"}