View in EDS

Constraints on the Feasibility of Ferrovolcanism on Asteroid 16 Psyche.

Saved in:
Bibliographic Details
Title: Constraints on the Feasibility of Ferrovolcanism on Asteroid 16 Psyche.
Authors: Jorritsma, J. J.1,2 (AUTHOR) j.jorritsma@tudelft.nl, van Westrenen, W.1 (AUTHOR)
Source: Journal of Geophysical Research. Planets. Aug2025, Vol. 130 Issue 8, p1-26. 26p.
Subject Terms: *Silicate minerals, Buoyancy, Volcanism, Surface properties, Meteorite analysis, Solar system, Asteroids
Abstract: Asteroid 16 Psyche's surface appears to be highly metallic, but its bulk density suggests a silicate‐rich interior. Ferrovolcanism has been suggested to explain how a silicate‐rich body could develop a metallic surface. This requires trapping of light elements bearing iron‐rich metallic melt in a core solidifying from the outside inwards. The buoyancy of the lighter melt must then generate sufficient pressure to carry metal melt through the mantle and cover the surface. Here, we test whether sufficient pressure could have been generated on 16 Psyche in different scenarios. Core size, light element partitioning between mantle and core, and silicate mass loss are calculated for three meteoritic bulk compositional models (H‐chondrite, EH‐chondrite and mesosiderite) based on mantle density and mantle porosity combinations. The resulting core compositions are used to calculate excess pressure. Mantle density and porosity combinations leading to ferrovolcanism are constrained for each bulk composition. Iron‐rich bulk compositions with low light element abundances are favored. Mesosiderite bulk composition is most conducive to producing ferrovolcanism but does not naturally fit the ferrovolcanism framework. Primitive compositions are favored as the timing of ferrovolcanism is tied to the earlier stages of solar system formation. H‐chondrite model scenarios may produce ferrovolcanism but require high amounts of mass loss to be considered as a building block for Psyche. EH‐chondrite model scenarios are chemically not conducive to producing ferrovolcanism. Both confirmation and rejection of the ferrovolcanism hypothesis by upcoming observations from NASA's Psyche mission can therefore provide key new constraints on 16 Psyche origin and evolution scenarios. Plain Language Summary: Asteroid 16‐Psyche, the largest M‐type asteroid, appears to have a significant amount of metal on its surface. Its density is not high enough to be fully metallic which leads to questions on the origin of the metal‐rich surface. A recent hypothesis invokes ferrovolcanism as the responsible process. This mechanism starts with a metallic core and silicate mantle. If the core solidifies from the outside in, a solid outer core shell can encapsulate lighter metallic magma in the center. The density difference between the molten inner core and solid outer core generates a buoyant pressure that can break apart the outer core and the mantle, carrying molten metal to the surface. This work tests whether sufficient buoyant pressure can be generated for a variety of bulk compositions and mantle properties of Psyche. Core size, composition and density are calculated for each model to assess buoyant pressure generation. Bulk compositions with lower density struggle to produce sufficient excess pressure as the cores that can be produced are small, as a consequence of their low iron content. Higher density building blocks with high iron contents are more conducive to generating sufficient pressures to carry metallic melt from 16‐Psyche's inner core to the surface. Key Points: Boundary conditions to achieve ferrovolcanism on Psyche are quantifiedThe entire formation history of Psyche must be taken into account to assess the probability of these conditions being met [ABSTRACT FROM AUTHOR]
Copyright of Journal of Geophysical Research. Planets is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: GreenFILE
Description
Abstract:Asteroid 16 Psyche's surface appears to be highly metallic, but its bulk density suggests a silicate‐rich interior. Ferrovolcanism has been suggested to explain how a silicate‐rich body could develop a metallic surface. This requires trapping of light elements bearing iron‐rich metallic melt in a core solidifying from the outside inwards. The buoyancy of the lighter melt must then generate sufficient pressure to carry metal melt through the mantle and cover the surface. Here, we test whether sufficient pressure could have been generated on 16 Psyche in different scenarios. Core size, light element partitioning between mantle and core, and silicate mass loss are calculated for three meteoritic bulk compositional models (H‐chondrite, EH‐chondrite and mesosiderite) based on mantle density and mantle porosity combinations. The resulting core compositions are used to calculate excess pressure. Mantle density and porosity combinations leading to ferrovolcanism are constrained for each bulk composition. Iron‐rich bulk compositions with low light element abundances are favored. Mesosiderite bulk composition is most conducive to producing ferrovolcanism but does not naturally fit the ferrovolcanism framework. Primitive compositions are favored as the timing of ferrovolcanism is tied to the earlier stages of solar system formation. H‐chondrite model scenarios may produce ferrovolcanism but require high amounts of mass loss to be considered as a building block for Psyche. EH‐chondrite model scenarios are chemically not conducive to producing ferrovolcanism. Both confirmation and rejection of the ferrovolcanism hypothesis by upcoming observations from NASA's Psyche mission can therefore provide key new constraints on 16 Psyche origin and evolution scenarios. Plain Language Summary: Asteroid 16‐Psyche, the largest M‐type asteroid, appears to have a significant amount of metal on its surface. Its density is not high enough to be fully metallic which leads to questions on the origin of the metal‐rich surface. A recent hypothesis invokes ferrovolcanism as the responsible process. This mechanism starts with a metallic core and silicate mantle. If the core solidifies from the outside in, a solid outer core shell can encapsulate lighter metallic magma in the center. The density difference between the molten inner core and solid outer core generates a buoyant pressure that can break apart the outer core and the mantle, carrying molten metal to the surface. This work tests whether sufficient buoyant pressure can be generated for a variety of bulk compositions and mantle properties of Psyche. Core size, composition and density are calculated for each model to assess buoyant pressure generation. Bulk compositions with lower density struggle to produce sufficient excess pressure as the cores that can be produced are small, as a consequence of their low iron content. Higher density building blocks with high iron contents are more conducive to generating sufficient pressures to carry metallic melt from 16‐Psyche's inner core to the surface. Key Points: Boundary conditions to achieve ferrovolcanism on Psyche are quantifiedThe entire formation history of Psyche must be taken into account to assess the probability of these conditions being met [ABSTRACT FROM AUTHOR]
ISSN:21699097
DOI:10.1029/2024JE008811