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Estabilización del disco alrededor de beta Pictoris por un gas extremadamente rico en carbono

Aki Roberge¹, Paul D Feldman, Alycia J Weinberger

¹Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA. akir@milkyway.gsfc.nasa.gov

|June 9, 2006

Resumen

El gas en el disco de escombros de beta Pictoris es sorprendentemente rico en carbono. Esta alta abundancia de carbono explica la estabilidad del disco, lo que sugiere que se formó a partir de materiales inusuales y ricos en carbono.

Área de la Ciencia:

Ciencia exoplanetaria Ciencia de los exoplanetas.
Evolución del sistema estelar Evolución del sistema estelar
La astroquímica es astroquímica.

Sus antecedentes:

Beta Pictoris alberga un prominente disco de escombros en el borde, un objeto clave para estudiar la formación de planetas.
Estudios anteriores indicaron abundancias de gas cerca del Sol, en conflicto con la estabilidad observada del disco.

Objetivo del estudio:

Investigar la composición gaseosa del disco beta de Pictoris.
Resolver la discrepancia entre la composición del gas y la estabilidad del disco.

Principales métodos:

Detección de carbono ionizado (C II, C III) y gas de oxígeno neutro (O I).
Análisis de las abundancias elementales de gas dentro del disco.

Principales resultados:

Se detectaron carbono ionizado simple y doblemente y gas de oxígeno atómico neutro.
Se ha descubierto que el carbono es extremadamente sobreabundante en comparación con otros elementos.
La sobreabundancia de carbono explica la rotación kepleriana y la estabilidad del disco.

Conclusiones:

La estabilidad del disco de gas se atribuye a una significativa sobreabundancia de carbono.
Esta sobreabundancia sugiere que el gas se origina en material planetesimal más rico en carbono que los análogos del Sistema Solar.

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