Eclipsing binary science via the merging of transit and doppler exoplanet survey data - a case study with the marvels pilot project and SuperWASP

• Autor(a) principal: Fleming, S.W.
• Data de Publicação: 2011
• Outros Autores: Maxted, Pierre F.L., Hebb, Leslie, Stassun, Keivan G., Ge, Jian, Cargile, Phillip A., Ghezzi, Luan, De Lee, Nathan M., Wisniewski, J.P., Gary, Bruce L., Mello, Gustavo Frederico Porto de, Ferreira, Letícia D., Zhao, Bo, Anderson, D.R., Wan, Xiaoke, Hellier, C., Guo, Pengcheng, West, R.G., Mahadevan, Suvrath, Pollacco, Don, Lee, B.L., Collier Cameron, A., Van Eyken, Julian C., Skillen, Ian, Crepp, Justin R., Nguyen, D.C., Kane, Stephen R., Paegert, Martin, Costa, Luiz N. da, Maia, Marcio Antonio Geimba, Santiago, Basilio Xavier
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/108148
• topic: Eclipses; Espectroscopia; Efeito doppler; Binaries: eclipsing; Binaries: spectroscopic

Exoplanet transit and Doppler surveys discover many binary stars during their operation that can be used to conduct a variety of ancillary science. Specifically, eclipsing binary stars can be used to study the stellar mass–radius relationship and to test predictions of theoretical stellar evolution models. By cross-referencing 24 binary stars found in theMARVELS Pilot Project with SuperWASP photometry, we find two new eclipsing binaries, TYC 0272-00458-1 and TYC 1422-01328-1, whichwe use as case studies to develop a general approach to eclipsing binaries in survey data.TYC0272-00458-1 is a single-lined spectroscopic binary for whichwe calculate amass of the secondary and radii for both components using reasonable constraints on the primary mass through several different techniques. For a primary mass ofM1 = 0.92±0.1M ,we findM2 = 0.610±0.036M ,R1 = 0.932±0.076R , and R2 = 0.559 ± 0.102R , and find that both stars have masses and radii consistent with model predictions. TYC 1422-01328-1 is a triple-component system for which we can directly measure the masses and radii of the eclipsing pair. We find that the eclipsing pair consists of an evolved primary star (M1 = 1.163 ± 0.034M , R1 = 2.063 ± 0.058R ) and a G-type dwarf secondary (M2 = 0.905 ± 0.067M , R2 = 0.887 ± 0.037R ). We provide the framework necessary to apply this analysis to much larger data sets.