{"paper":{"title":"Magnetar-powered long gamma-ray bursts and connection to superluminous supernovae and fast radio bursts","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"Long gamma-ray bursts powered by magnetars exhibit a correlation where stronger magnetic fields correspond to shorter initial spin periods.","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Fa-Yin Wang, Ning Gai, Shuang-Xi Yi, Yan-Ke Tang, Yan-Kun Qu, Yu-Peng Yang, Yu-Qi Zhou","submitted_at":"2026-05-13T12:36:24Z","abstract_excerpt":"Based on X-ray afterglow observations from the Swift satellite, we construct a sample of 169 long gamma-ray bursts (LGRBs) exhibiting the canonical magnetar plateau signature, i.e., a plateau followed by a $t^{-2}$ decay. We derive the plateau luminosity $L_0$ and break time $t_b$ for each burst by performing Markov Chain Monte Carlo (MCMC) fits to the light curves, and estimate pseudo-redshifts for bursts lacking known redshifts via the Amati relation. The fundamental magnetar parameters are subsequently inferred: the surface polar magnetic field strength $B_p \\in [0.39,\\ 23.08] \\times 10^{15"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"We identify a significant correlation between B_p and P_0: B_p ∝ P_0^{0.83 ± 0.09} for the full sample and B_p ∝ P_0^{0.80 ± 0.16} for the known-redshift subsample, with GRB magnetars possessing systematically stronger magnetic fields than those powering SLSNe.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The X-ray plateau is produced by magnetar spin-down energy injection, and pseudo-redshifts estimated via the Amati relation are sufficiently accurate to derive reliable B_p and P_0 values.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"A sample of 169 magnetar-candidate long GRBs yields B_p proportional to P_0 to the power 0.83 and fields an order of magnitude stronger than those in superluminous supernovae.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"Long gamma-ray bursts powered by magnetars exhibit a correlation where stronger magnetic fields correspond to shorter initial spin periods.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"2151302b6f1784d63797bc807a2ee6abb371c7a61d39a11b790838081ad540f4"},"source":{"id":"2605.13440","kind":"arxiv","version":2},"verdict":{"id":"4ec172fa-ab35-4831-aa40-b3fc9eb88235","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-15T02:38:32.751589Z","strongest_claim":"We identify a significant correlation between B_p and P_0: B_p ∝ P_0^{0.83 ± 0.09} for the full sample and B_p ∝ P_0^{0.80 ± 0.16} for the known-redshift subsample, with GRB magnetars possessing systematically stronger magnetic fields than those powering SLSNe.","one_line_summary":"A sample of 169 magnetar-candidate long GRBs yields B_p proportional to P_0 to the power 0.83 and fields an order of magnitude stronger than those in superluminous supernovae.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The X-ray plateau is produced by magnetar spin-down energy injection, and pseudo-redshifts estimated via the Amati relation are sufficiently accurate to derive reliable B_p and P_0 values.","pith_extraction_headline":"Long gamma-ray bursts powered by magnetars exhibit a correlation where stronger magnetic fields correspond to shorter initial spin periods."},"references":{"count":93,"sample":[{"doi":"","year":2017,"title":"P., Abbott, R., Abbott, T","work_id":"cee4e211-f7f0-4119-97ce-429c1211d2fd","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2006,"title":"2006, MNRAS, 372, 1,","work_id":"c24181d8-511d-4bd1-965a-3f52b85a6975","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2019,"title":"2019, MNRAS, 486, 1, L46","work_id":"6d18644c-4c94-4b71-b85c-9a6d9267a10f","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2025,"title":"2013, ApJL, 774, 2, L23","work_id":"77c9a596-74ae-4530-aa81-3096297dc221","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2002,"title":"Bloom, J. S., Kulkarni, S. R., & Djorgovski, S. G. 2002, AJ, 123, 3,","work_id":"93a25824-982c-4e54-8cfe-5b449482ff69","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":93,"snapshot_sha256":"e904f37541ab6191330664b26d6528d8667d786a9f21d2a96173e5bebf84b090","internal_anchors":3},"formal_canon":{"evidence_count":2,"snapshot_sha256":"16cfaa1ccfccd0499148d2d81b75a42b6b033a16d482c593137fb9078a8e9fcd"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}