{"paper":{"title":"The fundamental parameters of the roAp star $\\gamma$ Equulei","license":"http://creativecommons.org/licenses/publicdomain/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. Marcotto, A. Roussel, A. Spang, C. Farrington, D. Bonneau, D. Mourard, H. McAlister, I. Brand\\~ao, I. Tallon-Bosc, J.M. Clausse, J. Sturmann, K. Perraut, L. Sturmann, M. Cunha, N. Turner, O. Chesneau, O. Delaa, Ph. B\\'erio, Ph. Stee, P.J. Goldfinger, T. ten Brummelaar","submitted_at":"2010-11-09T10:33:28Z","abstract_excerpt":"Physical processes working in the stellar interiors as well as the evolution of stars depend on some fundamental stellar properties, such as mass, radius, luminosity, and chemical abundances. A classical way to test stellar interior models is to compare the predicted and observed location of a star on theoretical evolutionary tracks in a H-R diagram. This requires the best possible determinations of stellar mass, radius, luminosity and abundances. To derive its fundamental parameters, we observed the well-known rapidly oscillating Ap star, $\\gamma$ Equ, using the visible spectro-interferometer"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1011.2028","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"}