{"paper":{"title":"Grids of rotating stellar models with masses between 1.0 and 3.0 Msun","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Shaolan Bi, Wuming Yang, Xiangcun Meng","submitted_at":"2012-12-07T00:48:30Z","abstract_excerpt":"We calculated a grid of evolutionary tracks of rotating models with masses between 1.0 and 3.0 $M_{\\odot}$ and a resolution $\\delta M \\leq 0.02$ $M_{\\odot}$, which can be used to study the effects of rotation on stellar evolutions and on the characteristics of star clusters. The value of $\\sim$2.05 $M_{\\odot}$ is a critical mass for the effects of rotation on stellar structure and evolution. For stars with $M >$ 2.05 $M_{\\odot}$, rotation leads to an increase in the convective core and prolongs the lifetime of main sequence (MS); rotating models evolve slower than non-rotating ones; the effect"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1212.1511","kind":"arxiv","version":1},"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"}