{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:OE53OX746Y4YXH4QF4NAA3CRB3","short_pith_number":"pith:OE53OX74","schema_version":"1.0","canonical_sha256":"713bb75ffcf6398b9f902f1a006c510ec1f5beed32a6c640b9c2deaffa19e0b3","source":{"kind":"arxiv","id":"1307.6516","version":1},"attestation_state":"computed","paper":{"title":"The resonance triplet at E_alpha = 4.5 MeV in the 40Ca(alpha,gamma)44Ti reaction","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"nucl-ex","authors_text":"Andreas Wagner, Antonio Caciolli, Arnd R. Junghans, Daniel Bemmerer, Detlev Degering, Dmitry Yakorev, Dorothea Schumann, Frans Munnik, Gy\\\"orgy Gy\\\"urky, Kai Zuber, Konrad Schmidt, Konstanze Boretzky, Marie-Luise Menzel, Michael Anders, Michele Marta, Mirco Dietz, Roland Hannaske, Ronald Schwengner, Rugard Dressler, Shavkat Akhmadaliev, Tam\\'as Sz\\\"ucs, Zolt\\'an Elekes, Zsolt F\\\"ul\\\"op","submitted_at":"2013-07-24T18:19:06Z","abstract_excerpt":"The 40Ca(alpha,gamma)44Ti reaction is believed to be the main production channel for the radioactive nuclide 44Ti in core-collapse supernovae. Radiation from decaying 44Ti has been observed so far for two supernova remnants, and a precise knowledge of the 44Ti production rate may help improve supernova models. The 40Ca(alpha,gamma)44Ti astrophysical reaction rate is determined by a number of narrow resonances. Here, the resonance triplet at E_alpha = 4497, 4510, and 4523 keV is studied both by activation, using an underground laboratory for the gamma counting, and by in-beam gamma spectrometry"},"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":"1307.6516","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-ex","submitted_at":"2013-07-24T18:19:06Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"59e4cd936b8ffa9c0b04709bcbaa597834acdce48645e76c3e92a1191f92742c","abstract_canon_sha256":"033af0f21889cc4802c8d61a98b40d93bba9bb2277c0735a5929475a7978bb1f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:16:05.575234Z","signature_b64":"byAIbFk9HBGShjsRJsYVXad9ASV/dsnL7RtpYjq+e4XNpjwRrRJoP9NXz/zV8ivWcro/n/a43fAjNU5Lbr0dBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"713bb75ffcf6398b9f902f1a006c510ec1f5beed32a6c640b9c2deaffa19e0b3","last_reissued_at":"2026-05-18T03:16:05.574711Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:16:05.574711Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The resonance triplet at E_alpha = 4.5 MeV in the 40Ca(alpha,gamma)44Ti reaction","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"nucl-ex","authors_text":"Andreas Wagner, Antonio Caciolli, Arnd R. Junghans, Daniel Bemmerer, Detlev Degering, Dmitry Yakorev, Dorothea Schumann, Frans Munnik, Gy\\\"orgy Gy\\\"urky, Kai Zuber, Konrad Schmidt, Konstanze Boretzky, Marie-Luise Menzel, Michael Anders, Michele Marta, Mirco Dietz, Roland Hannaske, Ronald Schwengner, Rugard Dressler, Shavkat Akhmadaliev, Tam\\'as Sz\\\"ucs, Zolt\\'an Elekes, Zsolt F\\\"ul\\\"op","submitted_at":"2013-07-24T18:19:06Z","abstract_excerpt":"The 40Ca(alpha,gamma)44Ti reaction is believed to be the main production channel for the radioactive nuclide 44Ti in core-collapse supernovae. Radiation from decaying 44Ti has been observed so far for two supernova remnants, and a precise knowledge of the 44Ti production rate may help improve supernova models. The 40Ca(alpha,gamma)44Ti astrophysical reaction rate is determined by a number of narrow resonances. Here, the resonance triplet at E_alpha = 4497, 4510, and 4523 keV is studied both by activation, using an underground laboratory for the gamma counting, and by in-beam gamma spectrometry"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1307.6516","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":"1307.6516","created_at":"2026-05-18T03:16:05.574790+00:00"},{"alias_kind":"arxiv_version","alias_value":"1307.6516v1","created_at":"2026-05-18T03:16:05.574790+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1307.6516","created_at":"2026-05-18T03:16:05.574790+00:00"},{"alias_kind":"pith_short_12","alias_value":"OE53OX746Y4Y","created_at":"2026-05-18T12:27:54.935989+00:00"},{"alias_kind":"pith_short_16","alias_value":"OE53OX746Y4YXH4Q","created_at":"2026-05-18T12:27:54.935989+00:00"},{"alias_kind":"pith_short_8","alias_value":"OE53OX74","created_at":"2026-05-18T12:27:54.935989+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1908.08945","citing_title":"Background in $\\gamma$-ray detectors and carbon beam tests in the Felsenkeller shallow-underground accelerator laboratory","ref_index":39,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3","json":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3.json","graph_json":"https://pith.science/api/pith-number/OE53OX746Y4YXH4QF4NAA3CRB3/graph.json","events_json":"https://pith.science/api/pith-number/OE53OX746Y4YXH4QF4NAA3CRB3/events.json","paper":"https://pith.science/paper/OE53OX74"},"agent_actions":{"view_html":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3","download_json":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3.json","view_paper":"https://pith.science/paper/OE53OX74","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1307.6516&json=true","fetch_graph":"https://pith.science/api/pith-number/OE53OX746Y4YXH4QF4NAA3CRB3/graph.json","fetch_events":"https://pith.science/api/pith-number/OE53OX746Y4YXH4QF4NAA3CRB3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3/action/storage_attestation","attest_author":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3/action/author_attestation","sign_citation":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3/action/citation_signature","submit_replication":"https://pith.science/pith/OE53OX746Y4YXH4QF4NAA3CRB3/action/replication_record"}},"created_at":"2026-05-18T03:16:05.574790+00:00","updated_at":"2026-05-18T03:16:05.574790+00:00"}