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La respuesta de la marea de Io excluye un océano de magma poco profundo.

R S Park1, R A Jacobson2, L Gomez Casajus3

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Área de la Ciencia:

  • Ciencias planetarias
  • La geofísica
  • La astronomía

Sus antecedentes:

  • La actividad volcánica de Io es impulsada por el calentamiento de marea de su órbita excéntrica alrededor de Júpiter.
  • Esta disipación de energía de las mareas ha llevado a teorías de un océano de magma subterráneo global en Io.
  • Un océano de magma global poco profundo aumentaría significativamente la deformación de la marea de Io.

Objetivo del estudio:

  • Para medir la deformación de la marea de Io usando datos de la nave espacial Juno.
  • Para cuantificar el número de amor de la marea gravitacional (k2) y el parámetro de disipación de marea (Q).
  • Para probar la hipótesis de un océano de magma global poco profundo en Io.

Principales métodos:

  • Análisis de los datos Doppler de las naves espaciales Juno y Galileo.
  • Integración de las observaciones astrométricas.
  • Cálculo del número de amor de la marea gravitacional (Re ((k2)) y el parámetro de disipación de marea (Q).

Principales resultados:

  • Se ha medido Re ((k2) = 0,125 ± 0,047 y Q = 11,4 ± 3,6.
  • Estos valores indican que la deformación de marea de Io es menor de lo esperado para un océano de magma global poco profundo.
  • Los resultados son consistentes con que Io posee un manto en su mayoría sólido.

Conclusiones:

  • Io no posee un océano de magma global poco profundo.
  • Las fuerzas de marea no conducen universalmente a la formación de océanos de magma.
  • El rápido ascenso de la fusión, la intrusión y la erupción pueden evitar la formación de océanos de magma incluso con un fuerte calentamiento de las mareas.