{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:HTS7F5SS7MLZMHUZ3HSN42DXHL","short_pith_number":"pith:HTS7F5SS","schema_version":"1.0","canonical_sha256":"3ce5f2f652fb17961e99d9e4de68773ae1f9d8c0b490e24f9dd19c9db4742a68","source":{"kind":"arxiv","id":"1810.03514","version":3},"attestation_state":"computed","paper":{"title":"Critical Tests Of Leading Gamma Ray Burst Theories","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Arnon Dar, Shlomo Dado","submitted_at":"2018-10-08T15:00:35Z","abstract_excerpt":"Although it has been established observationally beyond doubt that broad-line stripped envelope supernovae (SNe) of type Ic produce long duration gamma ray bursts (GRBs), that neutron star mergers produce short hard GRBs (SHBs), and that phase transition of neutron stars in high mass X-ray binaries (HMXBs) may produce SN-Less GRBs, their production mechanism is still debated. The two leading theoretical models of GRBs and their afterglows, the fireball model and the cannonball model, have been widely confronted with the mounting observational data on GRBs and SHBs during the last two decades. "},"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":"1810.03514","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2018-10-08T15:00:35Z","cross_cats_sorted":[],"title_canon_sha256":"5be9bd5b7c56a81334449c8e6c2554a723f9020610a78f146ed3cfd73f0b2c7a","abstract_canon_sha256":"f56ea00e4323ad589a0d4604f3508d52e80e94bfd0f64671a052b474a692eb29"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:36:30.318859Z","signature_b64":"N8Zvx/z2gORPvIeMbl0d50xtm0XGI+jHsqFAeQFiUKQ+7Syc7eR8mMmP6+1R/e8C9jnXytS2WaaaxnOsu6b6Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3ce5f2f652fb17961e99d9e4de68773ae1f9d8c0b490e24f9dd19c9db4742a68","last_reissued_at":"2026-07-05T04:36:30.318421Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:36:30.318421Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Critical Tests Of Leading Gamma Ray Burst Theories","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Arnon Dar, Shlomo Dado","submitted_at":"2018-10-08T15:00:35Z","abstract_excerpt":"Although it has been established observationally beyond doubt that broad-line stripped envelope supernovae (SNe) of type Ic produce long duration gamma ray bursts (GRBs), that neutron star mergers produce short hard GRBs (SHBs), and that phase transition of neutron stars in high mass X-ray binaries (HMXBs) may produce SN-Less GRBs, their production mechanism is still debated. The two leading theoretical models of GRBs and their afterglows, the fireball model and the cannonball model, have been widely confronted with the mounting observational data on GRBs and SHBs during the last two decades. "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.03514","kind":"arxiv","version":3},"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/1810.03514/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":"1810.03514","created_at":"2026-07-05T04:36:30.318478+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.03514v3","created_at":"2026-07-05T04:36:30.318478+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.03514","created_at":"2026-07-05T04:36:30.318478+00:00"},{"alias_kind":"pith_short_12","alias_value":"HTS7F5SS7MLZ","created_at":"2026-07-05T04:36:30.318478+00:00"},{"alias_kind":"pith_short_16","alias_value":"HTS7F5SS7MLZMHUZ","created_at":"2026-07-05T04:36:30.318478+00:00"},{"alias_kind":"pith_short_8","alias_value":"HTS7F5SS","created_at":"2026-07-05T04:36:30.318478+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1909.01277","citing_title":"Deciphering the AMS cosmic-ray positron flux","ref_index":9,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL","json":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL.json","graph_json":"https://pith.science/api/pith-number/HTS7F5SS7MLZMHUZ3HSN42DXHL/graph.json","events_json":"https://pith.science/api/pith-number/HTS7F5SS7MLZMHUZ3HSN42DXHL/events.json","paper":"https://pith.science/paper/HTS7F5SS"},"agent_actions":{"view_html":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL","download_json":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL.json","view_paper":"https://pith.science/paper/HTS7F5SS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.03514&json=true","fetch_graph":"https://pith.science/api/pith-number/HTS7F5SS7MLZMHUZ3HSN42DXHL/graph.json","fetch_events":"https://pith.science/api/pith-number/HTS7F5SS7MLZMHUZ3HSN42DXHL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL/action/storage_attestation","attest_author":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL/action/author_attestation","sign_citation":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL/action/citation_signature","submit_replication":"https://pith.science/pith/HTS7F5SS7MLZMHUZ3HSN42DXHL/action/replication_record"}},"created_at":"2026-07-05T04:36:30.318478+00:00","updated_at":"2026-07-05T04:36:30.318478+00:00"}