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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{19}

\title{Estudio sobre la sensibilidad de la tasa de pérdida de masa del planeta HD 209458b}

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\author{Villarreal D'Angelo C.S.\inst{1}, Schneiter E.M.\inst{1,2}, Costa A.\inst{1,2}, Vel\'azquez P.\inst{3}, 
         Raga A.\inst{3}, Esquivel A.\inst{3}}

\institute{Instituto de Astronomía Teórica y Experimental (CONICET-UNC) \and
  Facultad de Ciencias Físicas, Exactas y Naturales (UNC) \and 
  Instituto de Ciencias Nucleares (UNAM)}

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\abstract{En este trabajo se presenta un estudio hidrodinámico de los efectos que 
diferentes condiciones del viento estelar y distintas estructuras del viento planetario
producen sobre el valor de absorción en Ly$\alpha$.\\

Particularmente, nuestro estudio fue realizado sobre el sistema planetario HD 209458.
Hasta el momento, las observaciones de dicho sistema
muestran la ocurrencia de una disminución de la emisión en Ly$\alpha$ cuando el planeta 
transita su estrella madre. Tomando en cuenta dichos valores de absorción y por medio de 
simulaciones hidrodinámicas 3D se propusieron diferentes modelos de vientos estelares 
y planetarios.\\

Considerando un rango de velocidades del viento estelar 
$\sim$[$350-800$] km s$^{-1}$, un rango de temperatura coronal $\sim$ [$3-7$] $\times
10^{6}$ $^\circ \mathrm{K}$ y dos valores del índice politrópico $\Gamma\sim[1.01-1.13]$, 
al mismo tiempo que se mantiene fija 
la tasa de pérdida de masa estelar, los resultados muestran que la tasa de pérdida de masa 
planetaria, $\dot M_p$, debe encontrarse en el rango $\sim[3-5] \times 10^{10}$g s$^{-1}$ para 
dar cuenta de la absorción en Ly$\alpha$ observada.\\

Las partículas que escapan de la atmósfera planetaria pueden hacerlo en diversas condiciones, 
las cuales dan lugar a distintas esctructuras del viento planetario. 
Dos de ellas son, el escape a través de las regiones polares, el cual está asociado al proceso 
de reconexión, y el escape a través del hemisferio nocturno del planeta, producido por la 
existencia de un fuerte viento estelar que comprime la atmósfera planetaria e inhibe el escape 
por el hemisferio diurno. Los resultados de nuestras simulaciones muestran que estos dos tipos de viento
planetario producen una mayor absorción que el caso en el que el viento es isotrópico.
}

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%  Select the keywords that describe your contribution. They are mandatory,  %
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\keywords{planets and satellites: individual (HD 209458b) --- stars: winds --- (stars:) planetary systems --- planet–star interactions --- stars: emission-line, Ly$\alpha$}

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\mail{cvillarreal@oac.edu.ar}

\maketitle

\end{document}
