{"paper":{"title":"Determining the Best Method of Calculating the Large Frequency Separation For Stellar Models","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"Enrico Corsaro, Lucas S. Viani, Sarbani Basu, Warrick H. Ball, William J. Chaplin","submitted_at":"2019-05-20T20:25:29Z","abstract_excerpt":"Asteroseismology of solar-like oscillators often relies on the comparisons between stellar models and stellar observations in order to determine the properties of stars. The values of the global seismic parameters, $\\nu_\\mathrm{max}$ (the frequency where the smoothed amplitude of the oscillations peak) and $\\Delta \\nu$ (the large frequency separation), are frequently used in grid-based modeling searches. However, the methods by which $\\Delta \\nu$ is calculated from observed data and how $\\Delta \\nu$ is calculated from stellar models are not the same. Typically for observed stars, especially fo"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1905.08333","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"}