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Here we report the distributions of the values $\\alpha_X$, $\\beta_X$ and their difference for a sample of 315 Swift GRBs. This sample includes all Swift GRBs that were detected before August 1, 2012, whose X-ray afterglow extended well beyond 1 day and the estimated err"},"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":"1203.1228","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2012-03-06T15:34:15Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"8e8506d0e751c9f488aae9f0b9d17395fd962b31bb12583a801330639b43fa16","abstract_canon_sha256":"fe77bdb3cc12adddd76f10db57c124c0779c1bb889a443a3681943e76c380d3c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:58:14.236149Z","signature_b64":"SfRoxPH7KDJBLEJqdY4A5TZvOUG8023JYmAdoyoOyk7viRdeQYoJ+rko1Jl+eRNXbzXbOkYWlQBZB+5gJ7dGAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"16371648113d0bec8a98d8344c698aa8b613e9aee435b93c73ce26b3ace81fbd","last_reissued_at":"2026-05-18T01:58:14.235443Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:58:14.235443Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Correlated Spectral And Temporal Behaviour Of Late-Time Afterglows Of Gamma Ray Bursts","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.HE","authors_text":"Arnon Dar, Shlomo Dado","submitted_at":"2012-03-06T15:34:15Z","abstract_excerpt":"The cannonball (CB) model of gamma ray bursts (GRBs) predicts that the asymptotic behaviour of the spectral energy density of the X-ray afterglow of GRBs is a power-law in time and in frequency where the difference between the temporal and spectral power-law indexes, $\\alpha_X-\\beta_X$, is restricted to the values 0, 1/2 and 1. 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