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Evidencia isotópica de un volcanismo de larga duración en Io

Katherine de Kleer¹, Ery C Hughes^1,2, Francis Nimmo³

¹Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA.

Science (New York, N.Y.)

|April 18, 2024

Resumen

Júpiter también.

Área de la Ciencia:

Ciencias planetarias
Astroquímica
La geofísica

Sus antecedentes:

La luna de Júpiter Io exhibe un intenso volcanismo alimentado por el calentamiento de las mareas.
La composición isotópica del elemento volátil en Io ofrece información sobre su historia de desgasificación y pérdida de masa.
Comprender la evolución de Io requiere analizar su inventario volátil atmosférico.

Objetivo del estudio:

Para medir los isótopos de azufre y cloro en la atmósfera de Io.
Para restringir el historial de desgasificación y pérdida de masa de Io a través del análisis isotópico.
Para inferir la duración e intensidad de la actividad volcánica de Io.

Principales métodos:

Se utilizaron observaciones submilimétricas de la atmósfera de Io.
Se midieron los isótopos de azufre en dióxido de azufre gaseoso y monóxido de azufre.
Se midieron los isótopos de cloro en el cloruro de sodio y el cloruro de potasio en estado gaseoso.

Principales resultados:

La proporción de isótopos de azufre (34S/32S) está muy enriquecida (δ34S = +347 ± 86‰).
La proporción de isótopos de cloro (37Cl/35Cl) también está significativamente enriquecida (δ37Cl = +263 ± 88‰).
Io ha perdido el 94% de su azufre disponible, lo que indica una desgasificación sustancial.

Conclusiones:

Io ha experimentado una gran actividad volcánica durante la mayor parte de su historia.
Los enriquecimientos isotópicos observados sugieren pérdidas volátiles significativas en escalas de tiempo geológicas.
Las tasas de desgasificación y pérdida de masa pasadas pueden haber sido más altas que las actuales.

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