{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:CHITCP54QSVBXMMCJFI2VOTQAX","short_pith_number":"pith:CHITCP54","schema_version":"1.0","canonical_sha256":"11d1313fbc84aa1bb1824951aaba7005d62d04482a18588c20018794dbfffec5","source":{"kind":"arxiv","id":"1312.7701","version":2},"attestation_state":"computed","paper":{"title":"Gamma-Ray Burst Prompt Emission Light Curves and Power Density Spectra in the ICMART Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Bing Zhang, Bo Zhang","submitted_at":"2013-12-30T13:01:08Z","abstract_excerpt":"In this paper, we simulate the prompt emission light curves of gamma-ray bursts (GRBs) within the framework of the Internal-Collision-induced MAgnetic Reconnection and Turbulence (ICMART) model. This model applies to GRBs with a moderately-high magnetization parameter $\\sigma$ in the emission region. We show that this model can produce highly variable light curves with both fast and slow components. The rapid variability is caused by many locally Doppler-boosted mini-emitters due to turbulent magnetic reconnection in a moderately-high-$\\sigma$ flow. The run-away growth and subsequent depletion"},"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":"1312.7701","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2013-12-30T13:01:08Z","cross_cats_sorted":[],"title_canon_sha256":"3c3ecebaaf28436456d76310e0e10a225762bf712090b876ddeca3936015cc42","abstract_canon_sha256":"3ff42c696a17def887991f1fbdf3304fc1f8c55a9e0dcc6bffbdb86c3007908d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:45:35.201589Z","signature_b64":"RGtNxbN5xDTIt2Yt9Ky5PRwWJQyxoYCpqVtREf5vOU6/TzyuYDP16a6/a06DMDYW0Qq4nk3ETxJ3FtG0rMxFDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"11d1313fbc84aa1bb1824951aaba7005d62d04482a18588c20018794dbfffec5","last_reissued_at":"2026-05-18T01:45:35.200967Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:45:35.200967Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gamma-Ray Burst Prompt Emission Light Curves and Power Density Spectra in the ICMART Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Bing Zhang, Bo Zhang","submitted_at":"2013-12-30T13:01:08Z","abstract_excerpt":"In this paper, we simulate the prompt emission light curves of gamma-ray bursts (GRBs) within the framework of the Internal-Collision-induced MAgnetic Reconnection and Turbulence (ICMART) model. This model applies to GRBs with a moderately-high magnetization parameter $\\sigma$ in the emission region. We show that this model can produce highly variable light curves with both fast and slow components. The rapid variability is caused by many locally Doppler-boosted mini-emitters due to turbulent magnetic reconnection in a moderately-high-$\\sigma$ flow. The run-away growth and subsequent depletion"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1312.7701","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":"1312.7701","created_at":"2026-05-18T01:45:35.201063+00:00"},{"alias_kind":"arxiv_version","alias_value":"1312.7701v2","created_at":"2026-05-18T01:45:35.201063+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1312.7701","created_at":"2026-05-18T01:45:35.201063+00:00"},{"alias_kind":"pith_short_12","alias_value":"CHITCP54QSVB","created_at":"2026-05-18T12:27:40.988391+00:00"},{"alias_kind":"pith_short_16","alias_value":"CHITCP54QSVBXMMC","created_at":"2026-05-18T12:27:40.988391+00:00"},{"alias_kind":"pith_short_8","alias_value":"CHITCP54","created_at":"2026-05-18T12:27:40.988391+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.00239","citing_title":"On the Duration of Gamma-Ray Bursts","ref_index":91,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX","json":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX.json","graph_json":"https://pith.science/api/pith-number/CHITCP54QSVBXMMCJFI2VOTQAX/graph.json","events_json":"https://pith.science/api/pith-number/CHITCP54QSVBXMMCJFI2VOTQAX/events.json","paper":"https://pith.science/paper/CHITCP54"},"agent_actions":{"view_html":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX","download_json":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX.json","view_paper":"https://pith.science/paper/CHITCP54","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1312.7701&json=true","fetch_graph":"https://pith.science/api/pith-number/CHITCP54QSVBXMMCJFI2VOTQAX/graph.json","fetch_events":"https://pith.science/api/pith-number/CHITCP54QSVBXMMCJFI2VOTQAX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX/action/storage_attestation","attest_author":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX/action/author_attestation","sign_citation":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX/action/citation_signature","submit_replication":"https://pith.science/pith/CHITCP54QSVBXMMCJFI2VOTQAX/action/replication_record"}},"created_at":"2026-05-18T01:45:35.201063+00:00","updated_at":"2026-05-18T01:45:35.201063+00:00"}