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La inestabilidad gravitacional en un disco de formación de planetas

Jessica Speedie1, Ruobing Dong2,3, Cassandra Hall4,5

  • 1Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia, Canada. jspeedie@uvic.ca.

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La inestabilidad gravitacional puede formar planetas directamente de los fragmentos de disco colapsados. La evidencia cinemática en el disco AB Aurigae apoya esta teoría de formación de planetas, lo que sugiere un disco masivo en relación con su estrella.

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Área de la Ciencia:

  • Astronomía y astrofísica
  • Ciencias planetarias

Sus antecedentes:

  • Las teorías de formación de planetas incluyen la acreción del núcleo y la inestabilidad gravitacional.
  • La inestabilidad gravitacional requiere discos circumestelares masivos (relación de masa disco-estrella ~1:10) para formar planetas directamente de fragmentos en colapso.
  • Estimar la masa del disco es un desafío, pero la cinemática de los gases puede revelar la inestabilidad del disco.

Objetivo del estudio:

  • Para presentar evidencia cinemática de la inestabilidad gravitacional en el disco protoplanetario alrededor de AB Aurigae.
  • Para probar la hipótesis de que la inestabilidad gravitacional puede desencadenar la formación de planetas.

Principales métodos:

  • Observaciones profundas de la emisión de líneas de 13CO y C18O utilizando el Atacama Large Millimeter/submillimeter Array (ALMA).
  • Análisis de la estructura de velocidad del disco para detectar firmas cinemáticas de inestabilidad gravitacional.
  • Comparación cuantitativa de la cinemática observada con las simulaciones y modelos analíticos.

Principales resultados:

  • Se detectó evidencia cinemática de inestabilidad gravitacional en el disco AB Aurigae.
  • Las estructuras de velocidad observadas coinciden estrechamente con las predicciones de los modelos teóricos.
  • La masa del disco inferido es de hasta un tercio de la masa estelar dentro de una región de 1′′ a 5′′.

Conclusiones:

  • Los hallazgos apoyan la teoría de la inestabilidad gravitacional para la formación de planetas.
  • El disco AB Aurigae es lo suficientemente masivo como para ser gravitatoriamente inestable.
  • La formación directa de protoplanetas a través de la fragmentación del disco es plausible en tales discos masivos.