{"paper":{"title":"General Relativistic Instability Supernova of a Supermassive Population III Star","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"2), (2) UMinn, (3) Monash, (4) LBNL, (5) LANL, 6), (6) ITA), Alexander Heger (3), Ann Almgren (4), Daniel Whalen (5, Jarrett Johnson (5) ((1) UCSC, Ke-Jung Chen (1, Stan Woosley (1)","submitted_at":"2014-02-19T19:24:57Z","abstract_excerpt":"The formation of supermassive Population III stars with masses $\\gtrsim$ 10,000 Msun in primeval galaxies in strong UV backgrounds at $z \\sim$ 15 may be the most viable pathway to the formation of supermassive black holes by $z \\sim$ 7. Most of these stars are expected to live for short times and then directly collapse to black holes, with little or no mass loss over their lives. But we have now discovered that non-rotating primordial stars with masses close to 55,000 Msun can instead die as highly energetic thermonuclear supernovae powered by explosive helium burning, releasing up to 10$ ^{55"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1402.4777","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"}