{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:EY3P56D5CEVMY7R5QAULDMGN5C","short_pith_number":"pith:EY3P56D5","schema_version":"1.0","canonical_sha256":"2636fef87d112acc7e3d8028b1b0cde8af0efbb20957a6bd2edcf2233a1af6cd","source":{"kind":"arxiv","id":"1811.06486","version":2},"attestation_state":"computed","paper":{"title":"Searching for the most powerful thermonuclear X-ray bursts with the Neil Gehrels Swift Observatory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"D.M. Palmer (LANL), J.J.M. in 't Zand (SRON), M.J.W. Kries (SRON & UU), N. Degenaar (UvA)","submitted_at":"2018-11-15T17:23:09Z","abstract_excerpt":"We searched for thermonuclear X-ray bursts from Galactic neutron stars in all event mode data of the Neil Gehrels Swift Observatory collected until March 31, 2018. In particular, we are interested in the intermediate-duration bursts (shell flashes fueled by thick helium piles) with the ill-understood phenomenon of strong flux fluctuations. Nine such bursts have been discussed in the literature to date. Swift is particularly suitable for finding additional examples. We find and list a total of 134 X-ray bursts; 44 are detected with BAT only, 41 with XRT only, and 49 with both. Twenty-eight burs"},"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":"1811.06486","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2018-11-15T17:23:09Z","cross_cats_sorted":[],"title_canon_sha256":"1914530beb1b51feeb5e7b5a4df7abb50269e781bed9487158b305bf62577a06","abstract_canon_sha256":"70086bbef1c7f318465b44e98ce0936e5490588a158d626dc2028a8d530ebdaa"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:56:16.967856Z","signature_b64":"Yb9hJmYYhTvd9/8qLpWrHHkFZQU5RYiYP9DPfwRXa7F/z0sTGqK0iCU54/jHwNQDtKq5OE4njOLoxngh9pryBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2636fef87d112acc7e3d8028b1b0cde8af0efbb20957a6bd2edcf2233a1af6cd","last_reissued_at":"2026-05-17T23:56:16.967327Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:56:16.967327Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Searching for the most powerful thermonuclear X-ray bursts with the Neil Gehrels Swift Observatory","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"D.M. Palmer (LANL), J.J.M. in 't Zand (SRON), M.J.W. Kries (SRON & UU), N. Degenaar (UvA)","submitted_at":"2018-11-15T17:23:09Z","abstract_excerpt":"We searched for thermonuclear X-ray bursts from Galactic neutron stars in all event mode data of the Neil Gehrels Swift Observatory collected until March 31, 2018. In particular, we are interested in the intermediate-duration bursts (shell flashes fueled by thick helium piles) with the ill-understood phenomenon of strong flux fluctuations. Nine such bursts have been discussed in the literature to date. Swift is particularly suitable for finding additional examples. We find and list a total of 134 X-ray bursts; 44 are detected with BAT only, 41 with XRT only, and 49 with both. Twenty-eight burs"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1811.06486","kind":"arxiv","version":2},"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":"1811.06486","created_at":"2026-05-17T23:56:16.967414+00:00"},{"alias_kind":"arxiv_version","alias_value":"1811.06486v2","created_at":"2026-05-17T23:56:16.967414+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1811.06486","created_at":"2026-05-17T23:56:16.967414+00:00"},{"alias_kind":"pith_short_12","alias_value":"EY3P56D5CEVM","created_at":"2026-05-18T12:32:22.470017+00:00"},{"alias_kind":"pith_short_16","alias_value":"EY3P56D5CEVMY7R5","created_at":"2026-05-18T12:32:22.470017+00:00"},{"alias_kind":"pith_short_8","alias_value":"EY3P56D5","created_at":"2026-05-18T12:32:22.470017+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.14264","citing_title":"The compact neutron star in 4U 1746-37 revisited: Reassessing the mass and radius","ref_index":79,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C","json":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C.json","graph_json":"https://pith.science/api/pith-number/EY3P56D5CEVMY7R5QAULDMGN5C/graph.json","events_json":"https://pith.science/api/pith-number/EY3P56D5CEVMY7R5QAULDMGN5C/events.json","paper":"https://pith.science/paper/EY3P56D5"},"agent_actions":{"view_html":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C","download_json":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C.json","view_paper":"https://pith.science/paper/EY3P56D5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1811.06486&json=true","fetch_graph":"https://pith.science/api/pith-number/EY3P56D5CEVMY7R5QAULDMGN5C/graph.json","fetch_events":"https://pith.science/api/pith-number/EY3P56D5CEVMY7R5QAULDMGN5C/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C/action/storage_attestation","attest_author":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C/action/author_attestation","sign_citation":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C/action/citation_signature","submit_replication":"https://pith.science/pith/EY3P56D5CEVMY7R5QAULDMGN5C/action/replication_record"}},"created_at":"2026-05-17T23:56:16.967414+00:00","updated_at":"2026-05-17T23:56:16.967414+00:00"}