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Title:
The Pre-Main-Sequence Eclipsing Binary TY Coronae Australis: Precise Stellar Dimensions and Tests of Evolutionary Models
Authors:
Casey, Brian W.; Mathieu, Robert D.; Vaz, Luiz Paulo R.; Andersen, Johannes; Suntzeff, Nicholas B.
Affiliation:
AA(Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706-1582 ), AB(Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706-1582 ), AC(Departamento de Física, Instituto de Ciências Exatas, Universidade Federal de Minas Gerais, C.P. 702, 30161-970 Belo Horizonte, MG, Brazil; ), AD(Astronomical Observatory, Niels Bohr Institute for Astronomy, Physics, and Geophysics, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark; ), AE(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories,1 Casilla 603, La Serena, Chile; )
Publication:
The Astronomical Journal, Volume 115, Issue 4, pp. 1617-1633. (AJ Homepage)
Publication Date:
04/1998
Origin:
AJ
AJ Keywords:
STARS: BINARIES: ECLIPSING, STARS: EVOLUTION, STARS: INDIVIDUAL: CONSTELLATION NAME: TY CORONAE AUSTRALIS
AJ/ApJ Keywords:
BINARIES: ECLIPSING, STARS: EVOLUTION, STARS: INDIVIDUAL: TY CORONAE AUSTRALIS
DOI:
10.1086/300270
Bibliographic Code:
1998AJ....115.1617C

Abstract

We analyze new photometric data for the Herbig Be eclipsing binary TY CrA, which securely reveal the secondary eclipse, ~0.03 mag deep in y. From the light-curve solution and our previous spectroscopic data, absolute dimensions of the primary and secondary stars are derived. The masses are found to be M_1 = 3.16 +/- 0.02 M_ȯ and M_2 = 1.64 +/- 0.01 M_ȯ, the radii are R_1 = 1.80 +/- 0.10 R_ȯ and R_2 = 2.08 +/- 0.14 R_ȯ, the luminosities are L_1 = 67 +/- 12 L_ȯ and L_2 = 2.4 +/- 0.8 L_ȯ, and the effective temperatures are T_1 = 12,000 +/- 500 K and T_2 = 4900 +/- 400 K. Here the uncertainties represent high-confidence limits, not standard deviations. The secondary star is a pre-main-sequence star located at the base of the Hayashi tracks. As such, it is the least evolved star with a dynamically measured mass. Given higher effective temperatures for the primary (e.g., 12,500 K), the solar-composition 1.64 M_ȯ evolutionary tracks of Swenson et al., Claret, and D'Antona & Mazzitelli are all consistent with the properties of the TY CrA secondary and suggest an age of order 3 Myr. The radius and projected rotational velocity of the secondary star are consistent with synchronous rotation. The primary star is located near the zero-age main sequence, which, for solar compositions, is consistent with an age of 3 Myr. However, the primary star is not well represented by any of the 3.16 M_ȯ evolutionary models, which predict somewhat higher effective temperatures than observed.
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