{"paper":{"title":"Isochrones for Old (> 5 Gyr) Stars and Stellar Populations. I. Models for $-2.4 \\le$ [Fe/H] $\\le +0.6$, $0.25 \\le Y \\le 0.33$, and $-0.4 \\le$ [$\\alpha$\\Fe] $\\le +0.4$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Bengt Edvardsson, Don A. VandenBerg, Jason W. Ferguson, Peter A. Bergbusch","submitted_at":"2014-09-03T23:26:11Z","abstract_excerpt":"Canonical grids of stellar evolutionary sequences have been computed for the helium mass-fraction abundances $Y = 0.25$, $0.29$, and $0.33$, and for iron abundances that vary from $-2.4$ to $+0.4$ (in 0.2 dex increments) when [$\\alpha$/Fe] $= +0.4$, or for the ranges $-2.0 \\le$ [Fe/H] $\\le +0.6$, $-1.8 \\le$ [Fe/H] $\\le +0.6$ when [$\\alpha$/Fe] $= 0.0$ and $-0.4$, respectively. The grids, which consist of tracks for masses from $0.12 {{\\cal M}_\\odot}$ to $1.1$-$1.5 {{\\cal M}_\\odot}$ (depending on the metallicity) are based on up-to-date physics, including the gravitational settling of helium (b"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1409.1283","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"}