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Dos familias de exocometas en el sistema β Pictoris

F Kiefer¹, A Lecavelier des Etangs², J Boissier³

¹1] Centre National de la Recherche Scientifique (CNRS), Unité Mixte de Recherche (UMR) 7095, Institut d'Astrophysique de Paris, 98 bis boulevard Arago, F-75014 Paris, France [2] Université Pierre et Marie Curie, UMR 7095, Institut d'Astrophysique de Paris, 98 bis boulevard Arago, F-75014 Paris, France [3] School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel.

|October 25, 2014

Resumen

Los cuerpos menores activos como los asteroides y los cometas en el joven sistema β Pictoris producen polvo y gas. El análisis revela dos poblaciones de exocometas, una agotada y otra recientemente fragmentada, análogas a los cometas de nuestro Sistema Solar.

Área de la Ciencia:

La ciencia exoplanetaria es la ciencia de los exoplanetas.
Evolución del sistema estelar en la evolución del sistema estelar.
La astroquímica es astroquímica.

Sus antecedentes:

El joven sistema planetario β Pictoris alberga cuerpos menores activos, análogos a los primeros procesos del Sistema Solar.
Estos cuerpos, incluidos los asteroides y los cometas, generan sustancial polvo y gas a través de colisiones y evaporación.
Las observaciones espectroscópicas anteriores indicaron tránsitos frecuentes de cuerpos pequeños y evaporados, llamados exocometas.

Objetivo del estudio:

Para analizar datos espectroscópicos de archivo de β Pictoris para caracterizar las poblaciones de exocometas.
Para investigar las propiedades físicas y los orígenes de los exocometas que transitan por el disco β Pictoris.
Para comparar los exocometas observados con cuerpos cometarios en nuestro Sistema Solar.

Principales métodos:

Análisis de más de 1.000 espectros de archivo recogidos entre 2003 y 2011.
Identificación y análisis estadístico de aproximadamente 6.000 firmas de absorción variable de exocometas en tránsito.
Categoría de los exocometas basada en la profundidad de la línea de absorción y las propiedades físicas.

Principales resultados:

Se identificaron dos poblaciones distintas de exocometas en el sistema β Pictoris.
Una población exhibe líneas de absorción poco profundas, lo que sugiere cometas viejos y agotados en resonancia con un planeta masivo.
La segunda población muestra líneas de absorción profundas, lo que podría indicar una fragmentación reciente de los cuerpos padres.

Conclusiones:

Los cuerpos de evaporación observados en el sistema β Pictoris son análogos a los cometas que se encuentran en nuestro Sistema Solar.
El estudio proporciona información sobre la composición y la dinámica de los cuerpos menores en sistemas planetarios jóvenes.
Las dinámicas de resonancia y los eventos de fragmentación parecen dar forma a las poblaciones de exocometas.

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