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Un sistema binario que interactúa con los poderes de procesamiento de las salidas de una estrella evolucionada.

Henri M J Boffin1, Brent Miszalski, Thomas Rauch

  • 1European Southern Observatory (ESO), Casilla 19001, Santiago, Chile. hboffin@eso.org

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|November 10, 2012
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Las interacciones de las estrellas binarias, específicamente un disco de acreción de precesión, probablemente explican las formas no esféricas de las nebulosas planetarias. Este estudio confirma este escenario en el sistema Fleming 1, sugiriéndolo.

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Área de la Ciencia:

  • La astronomía y la astrofísica.
  • Evolución Estelar Evolución Estelar
  • Sistemas de estrellas binarias sistemas estelares binarios.

Sus antecedentes:

  • Las estrellas suelen aparecer esféricas, pero sus envolturas expulsadas durante las últimas etapas de la vida, particularmente en la fase de nebulosa planetaria, a menudo exhiben formas no esféricas.
  • Las salidas asimétricas se observan comúnmente en las nebulosas planetarias, lo que lleva a investigar sus orígenes.

Objetivo del estudio:

  • Para investigar el papel de las interacciones de estrellas binarias en la formación de nebulosas planetarias.
  • Confirmar el mecanismo propuesto de un disco de acreción de precesión que lanza chorros simétricos de punto en el sistema Fleming 1.

Principales métodos:

  • Análisis de observación del sistema Fleming 1.
  • Identificación de un núcleo binario con envoltura posterior a la común.

Principales resultados:

  • Se confirmó que el sistema Fleming 1 alberga un núcleo binario de sobre post-común.
  • Este hallazgo apoya la hipótesis de que las interacciones binarias son responsables de la asimetría observada en las nebulosas planetarias.

Conclusiones:

  • La presencia de un núcleo binario de envoltura post-común en Fleming 1 favorece fuertemente el escenario de interacciones binarias que causan salidas asimétricas.
  • Este mecanismo es probablemente aplicable a una amplia gama de otros sistemas de nebulosas planetarias que exhiben características similares.