{"paper":{"title":"Light equation in eclipsing binary CV Boo: third body candidate in elliptical orbit","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.SR","authors_text":"A. I. Bogomazov, A.V. Khalikova, A. V. Tutukov, B. L. Satovskii, M. A. Ibrahimov, R.G. Karimov, Sh. A. Ehgamberdiev, T. R. Irsmambetova, V. N. Krushevska, V. S. Kozyreva, Yu. G. Kuznyetsova","submitted_at":"2016-11-14T21:44:10Z","abstract_excerpt":"A short period eclipsing binary star CV Boo is tested for the possible existence of additional bodies in the system with a help of the light equation method. We use data on the moments of minima from the literature as well as from our observations during 2014 May--July. A variation of the CV Boo's orbital period is found with a period of $\\approx 75$ d. This variation can be explained by the influence of a third star with a mass of $\\approx 0.4M_{\\odot}$ in an eccentric orbit with $e\\approx 0.9$. A possibility that the orbital period changes on long time scales is discussed. The suggested tert"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1611.04627","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"}