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A basal magma ocean dynamo to explain the early lunar magnetic field.

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Title: A basal magma ocean dynamo to explain the early lunar magnetic field.
Authors: Scheinberg, Aaron L.1 scheinberg@princeton.edu, Soderlund, Krista M.2, Elkins-Tanton, Linda T.3
Source: Earth & Planetary Science Letters. Jun2018, Vol. 492, p144-151. 8p.
Subjects: Magnetic fields, Magnetic flux density, Magmas, Convection (Astrophysics), Lunar heat flow
Abstract: The source of the ancient lunar magnetic field is an unsolved problem in the Moon's evolution. Theoretical work invoking a core dynamo has been unable to explain the magnitude of the observed field, falling instead one to two orders of magnitude below it. Since surface magnetic field strength is highly sensitive to the depth and size of the dynamo region, we instead hypothesize that the early lunar dynamo was driven by convection in a basal magma ocean formed from the final stages of an early lunar magma ocean; this material is expected to be dense, radioactive, and metalliferous. Here we use numerical convection models to predict the longevity and heat flow of such a basal magma ocean and use scaling laws to estimate the resulting magnetic field strength. We show that, if sufficiently electrically conducting, a magma ocean could have produced an early dynamo with surface fields consistent with the paleomagnetic observations. [ABSTRACT FROM AUTHOR]
Copyright of Earth & Planetary Science Letters is the property of Elsevier B.V. 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.)
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  Data: <searchLink fieldCode="AR" term="%22Scheinberg%2C+Aaron+L%2E%22">Scheinberg, Aaron L.</searchLink><relatesTo>1</relatesTo><i> scheinberg@princeton.edu</i><br /><searchLink fieldCode="AR" term="%22Soderlund%2C+Krista+M%2E%22">Soderlund, Krista M.</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Elkins-Tanton%2C+Linda+T%2E%22">Elkins-Tanton, Linda T.</searchLink><relatesTo>3</relatesTo>
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  Data: <searchLink fieldCode="JN" term="%22Earth+%26+Planetary+Science+Letters%22">Earth & Planetary Science Letters</searchLink>. Jun2018, Vol. 492, p144-151. 8p.
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  Data: <searchLink fieldCode="DE" term="%22Magnetic+fields%22">Magnetic fields</searchLink><br /><searchLink fieldCode="DE" term="%22Magnetic+flux+density%22">Magnetic flux density</searchLink><br /><searchLink fieldCode="DE" term="%22Magmas%22">Magmas</searchLink><br /><searchLink fieldCode="DE" term="%22Convection+%28Astrophysics%29%22">Convection (Astrophysics)</searchLink><br /><searchLink fieldCode="DE" term="%22Lunar+heat+flow%22">Lunar heat flow</searchLink>
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  Data: The source of the ancient lunar magnetic field is an unsolved problem in the Moon's evolution. Theoretical work invoking a core dynamo has been unable to explain the magnitude of the observed field, falling instead one to two orders of magnitude below it. Since surface magnetic field strength is highly sensitive to the depth and size of the dynamo region, we instead hypothesize that the early lunar dynamo was driven by convection in a basal magma ocean formed from the final stages of an early lunar magma ocean; this material is expected to be dense, radioactive, and metalliferous. Here we use numerical convection models to predict the longevity and heat flow of such a basal magma ocean and use scaling laws to estimate the resulting magnetic field strength. We show that, if sufficiently electrically conducting, a magma ocean could have produced an early dynamo with surface fields consistent with the paleomagnetic observations. [ABSTRACT FROM AUTHOR]
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  Data: <i>Copyright of Earth & Planetary Science Letters is the property of Elsevier B.V. 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.</i> (Copyright applies to all Abstracts.)
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        Value: 10.1016/j.epsl.2018.04.015
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      – Code: eng
        Text: English
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      – SubjectFull: Magnetic fields
        Type: general
      – SubjectFull: Magnetic flux density
        Type: general
      – SubjectFull: Magmas
        Type: general
      – SubjectFull: Convection (Astrophysics)
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      – SubjectFull: Lunar heat flow
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      – TitleFull: A basal magma ocean dynamo to explain the early lunar magnetic field.
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              Text: Jun2018
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