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Centro de Astrofísica da Universidade do Porto

The eclipsing binary TY CrA revisited: What near-IR light curves tell us

M. Vaňko, M. Ammler-von Eiff, T. Pribulla, R. Chini, E. Covino, R. Newhäuser

Abstract
New photometric observations of the hierarchical eclipsing TYCrA system were taken in the optical with VYSOS6 and in the near-IR with SOFI and REMIR. They are the first observations showing the deep eclipse minimum of the pre-main sequence secondary in the near-IR. For the first time, the secondary minimum can be reliably used in the calculation of the O-C diagram of TYCrA. By now, the O-C diagram can be studied on a time basis of about two decades. We confirm, that the O-C diagram cannot be explained by the spectroscopic tertiary. For the first time, the light curve of the inner eclipsing binary is analysed in both optical and near-IR bands simultaneously. In combination with already published spectroscopic elements, precise absolute dimensions and masses of the primary and the secondary component are obtained using the ROCHE code. The inclusion of the near-IR data puts strong constraints on the third light which is composed of the reflection nebula, the spectroscopic tertiary and a visual fourth component. The absolute parameters of the inner eclipsing binary agree very well with previous work except of the primary radius (1.46 ± 0.15 R) and luminosity (40 ± 10 L) which are clearly smaller. While the parameters of the secondary are well understood when assuming an age of about 3-5Myrs, the primary seems considerably undersized. Low metallicity cannot explain the parameters of the primary.

Keywords
binaries: eclipsing – stars: pre-main sequence – stars: evolution – stars: fundamental parameters.

Notes
Based on observations taken at the University Observatory of Bochum at Cerro Armazones, Chile. Based on observations made with the REM Telescope, INAF Chile under programmes 19002, 21024, and 23015. Based on observations collected at the European Southern Observatory, Chile (programme 77.C-0549).

Monthly Notices of the Royal Astronomical Society
Volume 431, Page 2230
May 2013

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