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Simulation of the Planetary Interior Differentiation Processes in the Laboratory
Published on: November 15, 2013
Elementos radiactivos en la superficie de Mercurio de MESSENGER: implicaciones para la formación y evolución del
Patrick N Peplowski1, Larry G Evans, Steven A Hauck
1The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. patrick.peplowski@jhuapl.edu
Science (New York, N.Y.)
|October 1, 2011
Resumen
El Mensajero de Dios.
Área de la Ciencia:
- Ciencias planetarias Ciencias planetarias.
- La geoquímica es la geoquímica.
- La astrofísica nuclear es una astrofísica nuclear.
Sus antecedentes:
- La composición de la superficie de Mercurio proporciona pistas sobre su formación y evolución.
- Los elementos radiactivos como el potasio (K), el torio (Th) y el uranio (U) son indicadores clave de los procesos planetarios.
Objetivo del estudio:
- Para determinar la abundancia superficial de K, Th y U en el hemisferio norte de Mercurio.
- Utilizar estas abundancias para limitar los modelos de la formación de Mercurio y su historia térmica.
Principales métodos:
- Se utilizaron datos del espectrómetro de rayos gamma MESSENGER.
- Abundancias superficiales medias medidas de K, Th y U en el hemisferio norte de Mercurio.
Principales resultados:
- Abundancias superficiales promedio: K (1150 ± 220 partes por millón), Th (220 ± 60 partes por millón), U (90 ± 20 partes por millón).
- Las relaciones K/Th y K/U sugieren la formación de material rico en volátiles, no el calentamiento extremo.
- Las abundancias indican una disminución significativa en la producción de calor interno desde la formación.
Conclusiones:
- El mercurio probablemente se formó a partir de materiales volátiles similares a los meteoritos condríticos.
- El vulcanismo generalizado ocurrió temprano en la historia de Mercurio, seguido de una actividad reducida.
- Estos hallazgos desafían los modelos que requieren un calentamiento planetario extremo durante la formación.
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