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Multiwavelength Photometry of the Young Intermediate Mass Eclipsing Binary TY CrA

Published online by Cambridge University Press:  23 April 2012

M. Ammler-von Eiff ,
M. Vaňko ,
T. Pribulla ,
E. Covino ,
R. Neuhäuser  and
V. Joergens
M. Ammler-von Eiff
Affiliation:
Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany email: [email protected]
M. Vaňko
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia email: [email protected], [email protected]
T. Pribulla
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia email: [email protected], [email protected]
E. Covino
Affiliation:
INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16 80131 - Napoli, Italy
R. Neuhäuser
Affiliation:
Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergäßchen 2-3, 07745 Jena, Germany
V. Joergens
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany Zentrum für Astronomie Heidelberg, Institut für Theoretische Astrophysik Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
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Abstract

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One of the handful of known PMS eclipsing binaries is a component of the spectroscopic triple TY CrA. Its secondary component is particularly interesting since it is a star of relatively high mass (1.64 M⊙) which is still on the pre-main sequence. The eclipsing binary was analyzed in the optical wavelength range ~10 years ago, however, the crucial secondary eclipse minimum is very shallow. Therefore, we are obtaining new photometry in both optical and near-IR bands. We present first observations in (BVRI) which show that the secondary eclipse depth increases to about 0.1 mag in the I band. The increased eclipse depth with respect to other bands will help to better determine the colours and dimensions of the system. Furthermore, we show and discuss first near-IR observations of the primary eclipse. In addition to the light curves we are obtaining radial velocities in order to pin down the orbital parameters of the triple. Our first observations agree with the orbital parameters derived ~10 years ago.

Keywords

binaries: eclipsingstars: fundamental parametersstars: individual (TY CrA) etc.
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 59 - 60
Copyright
Copyright © International Astronomical Union 2012

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