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\documentclass[craaa]{aaa2014}

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\usepackage[spanish,activeacute,english]{babel}
\usepackage[utf8]{inputenc}
\usepackage{verbatim}
\usepackage{amsmath}
\usepackage{amsfonts}
\usepackage{amssymb}

\begin{document}

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\journalvol{57}
\journalyear{2014}
\journaleditors{A.C. Rovero, C. Beaugé, L.J. Pellizza, M. Lares}

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\contriblanguage{0}

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\contribtype{2}

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%  11 [AEC]: Astrofísica Extragaláctica y Cosmología /                       %
%           Extragalactic Astrophysics and Cosmology                         %
%  12 [EG]: Estructura Galáctica / Galactic Structure                        %
%  13 [AE]: Astrofísica Estelar / Stellar Astrophysics                       %
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\thematicarea{14}

\title{An\'alisis de  binaria masiva eclipsante MTT58}

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\author{Jaque Arancibia M.\inst{1}, Barb\'a R.H.\inst{2}, Morrell N.\inst{3}}

\institute{Instituto de Ciencias Astron\'omicas, de la Tierra y del Espacio (ICATE-CONICET), Argentina \and
  Universidad de La Serena, Chile \and 
  Las Campanas Observatory, Chile}

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\abstract{El cúmulo estelar masivo
NGC 3603 es un sitio privilegiado en la V\'ia L\'actea para llevar a cabo estudios sobre la formaci\'on y evoluci\'on de las 
estrellas masivas. En dicho c\'umulo se hallan decenas de estrellas masivas de tipo  O y WN, algunas de las cuales pueden 
tener masas del orden de 100 a 150 masas solares. Ubicada en la periferia de este  conglomerado se encuentra la binaria 
masiva eclipsante MTT58, clasificada espectralmente como O2 If*/WN6. En este trabajo presentamos un an\'alisis de las curvas 
de luz en las bandas V y Hc, junto con la soluci\'on orbital derivada de velocidades radiales obtenidas en espectros 
observados en cuadraturas con el telescopio de 6.5-m Magallanes Clay. Estas soluciones de la curva de luz y de velocidad 
radial nos han permitido derivar parámetros absolutos del sistema. MTT 58 es la binaria de tipo O2-3.5 If*/WN 5-6 de m\'as 
corto per\'iodo conocido, 1.93 d\'ias, y las dimensiones f\'isicas de las estrellas indican radios m\'as peque\~nos que los
esperados para estrellas de este tipo espectral, lo cual puede aportar evidencia sobre la juventud del sistema. Dada la 
rareza de sistemas binarios eclipsantes  masivos, podemos afirmar que MTT58 se convertir\'a en un hito para la calibraci\'on 
de los modelos evolutivos de estrellas muy masivas.}

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\keywords{stars: massive --- binaries: eclipsing}

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\mail{mjaque@icate-conicet.gob.ar}

\maketitle

\end{document}
