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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

¹Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA. Ryan.S.Park@jpl.nasa.gov.

|December 12, 2024

Resumen

Yo también.

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.

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