{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:X2IYX2ACBVC5YMF3HEPOESGASQ","short_pith_number":"pith:X2IYX2AC","schema_version":"1.0","canonical_sha256":"be918be8020d45dc30bb391ee248c09433eb7abb775af7ade93544976a6c8a2c","source":{"kind":"arxiv","id":"0708.1970","version":1},"attestation_state":"computed","paper":{"title":"Pair creation supernovae at low and high redshift","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. de Koter, C. A. Norman, Jorick Vink, M. Cantiello, N. Langer, S.-C.Yoon","submitted_at":"2007-08-14T22:15:00Z","abstract_excerpt":"Pair creation supernovae (PCSN) are thought to be produced from very massive low metallicity stars. The spectacularly bright SN 2006gy does show signatures expected from PCSNe. Here, we investigate the metallicity threshold below which PCSN can form and estimate their occurrence rate. We perform stellar evolution calculations for stars of 150$\\mso$ and 250$\\mso$ of low metallicity (Z$_{\\odot}$/5 and Z$_{\\odot}$/20), and analyze their mass loss rates. We find that the bifurcation between quasi-chemically homogeneous evolution for fast rotation and conventional evolution for slower rotation, whi"},"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":"0708.1970","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-08-14T22:15:00Z","cross_cats_sorted":[],"title_canon_sha256":"eec87c32619be6ebf557fef77a32190dc0e6ff7f9db318bf498934922c09e295","abstract_canon_sha256":"b54190db9dcd54985a9fea125145f801c9515c0e03f8c66e6088312b8e0773d2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:05:11.079742Z","signature_b64":"+OWrrdI2v9spPhXqUxC4Kex9eC3b0PlhLyjiiSQy0RGcLMDsEHK5QTPkdFOVFzVZhomNzusWC6aN58CbS0AJCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"be918be8020d45dc30bb391ee248c09433eb7abb775af7ade93544976a6c8a2c","last_reissued_at":"2026-07-04T17:05:11.079341Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:05:11.079341Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Pair creation supernovae at low and high redshift","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. de Koter, C. A. Norman, Jorick Vink, M. Cantiello, N. Langer, S.-C.Yoon","submitted_at":"2007-08-14T22:15:00Z","abstract_excerpt":"Pair creation supernovae (PCSN) are thought to be produced from very massive low metallicity stars. The spectacularly bright SN 2006gy does show signatures expected from PCSNe. Here, we investigate the metallicity threshold below which PCSN can form and estimate their occurrence rate. We perform stellar evolution calculations for stars of 150$\\mso$ and 250$\\mso$ of low metallicity (Z$_{\\odot}$/5 and Z$_{\\odot}$/20), and analyze their mass loss rates. We find that the bifurcation between quasi-chemically homogeneous evolution for fast rotation and conventional evolution for slower rotation, whi"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0708.1970","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/0708.1970/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":"0708.1970","created_at":"2026-07-04T17:05:11.079401+00:00"},{"alias_kind":"arxiv_version","alias_value":"0708.1970v1","created_at":"2026-07-04T17:05:11.079401+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0708.1970","created_at":"2026-07-04T17:05:11.079401+00:00"},{"alias_kind":"pith_short_12","alias_value":"X2IYX2ACBVC5","created_at":"2026-07-04T17:05:11.079401+00:00"},{"alias_kind":"pith_short_16","alias_value":"X2IYX2ACBVC5YMF3","created_at":"2026-07-04T17:05:11.079401+00:00"},{"alias_kind":"pith_short_8","alias_value":"X2IYX2AC","created_at":"2026-07-04T17:05:11.079401+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.02725","citing_title":"Can current models predict the local black hole merger rate?","ref_index":84,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ","json":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ.json","graph_json":"https://pith.science/api/pith-number/X2IYX2ACBVC5YMF3HEPOESGASQ/graph.json","events_json":"https://pith.science/api/pith-number/X2IYX2ACBVC5YMF3HEPOESGASQ/events.json","paper":"https://pith.science/paper/X2IYX2AC"},"agent_actions":{"view_html":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ","download_json":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ.json","view_paper":"https://pith.science/paper/X2IYX2AC","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0708.1970&json=true","fetch_graph":"https://pith.science/api/pith-number/X2IYX2ACBVC5YMF3HEPOESGASQ/graph.json","fetch_events":"https://pith.science/api/pith-number/X2IYX2ACBVC5YMF3HEPOESGASQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ/action/storage_attestation","attest_author":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ/action/author_attestation","sign_citation":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ/action/citation_signature","submit_replication":"https://pith.science/pith/X2IYX2ACBVC5YMF3HEPOESGASQ/action/replication_record"}},"created_at":"2026-07-04T17:05:11.079401+00:00","updated_at":"2026-07-04T17:05:11.079401+00:00"}