2003
DOI: 10.1038/nature01267
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An early lunar core dynamo driven by thermochemical mantle convection

Abstract: Although the Moon currently has no internally generated magnetic field, palaeomagnetic data, combined with radiometric ages of Apollo samples, provide evidence for such a magnetic field from approximately 3.9 to 3.6 billion years (Gyr) ago, possibly owing to an ancient lunar dynamo. But the presence of a lunar dynamo during this time period is difficult to explain, because thermal evolution models for the Moon yield insufficient core heat flux to power a dynamo after approximately 4.2 Gyr ago. Here we show tha… Show more

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Cited by 176 publications
(163 citation statements)
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“…We use TERRA, a parallel, well-established, benchmarked, spherical convection code (Baumgardner, 1985;Bunge and Baumgardner, 1995;Yang and Baumgardner, 2000;Stegman et al, 2002Stegman et al, , 2003Köstler, 2011;Davies et al, 2013). The grid covers the full 3-D spherical shell.…”
Section: Numerical Mantle Convection Simulationsmentioning
confidence: 99%
See 1 more Smart Citation
“…We use TERRA, a parallel, well-established, benchmarked, spherical convection code (Baumgardner, 1985;Bunge and Baumgardner, 1995;Yang and Baumgardner, 2000;Stegman et al, 2002Stegman et al, , 2003Köstler, 2011;Davies et al, 2013). The grid covers the full 3-D spherical shell.…”
Section: Numerical Mantle Convection Simulationsmentioning
confidence: 99%
“…Numerical mantle convection codes have been developed that are capable of tracking chemical heterogeneities (for an overview see Tackley, 2007). Although different techniques each have advantages (level set -Samuel and Evonuk, 2010; field tracking - Davies et al, 2007; and marker-net based method - Oldham and Davies, 2004), particle-based methods have proven to be most useful for systems that involve strong mixing, e.g.…”
Section: Introductionmentioning
confidence: 99%
“…& Solomon, 1973;Stevenson et al, 1983;Konrad & Spohn, 1997;Stegman et al, 2003;Grimm, 2013;Laneuville et al, 2013). While the thermal evolution of the deep Moon depends on many factors (e.g., Evans et al, 2014), most model calculations suggest that the upper part of the Moon cooled rapidly (i.e., within several 100 Myr) unless the radiogenic heating rate was anomalously high at the 55 base of the crust (i.e., a 10-km thick layer with >10 ppm thorium concentration) (e.g., Wieczorek & Phillips, 2000).…”
mentioning
confidence: 99%
“…Rather, the dynamo was in the mantle as it cooled through the magma ocean phase after having developed an early crust (Stevenson 2001). Stegman et al (2003) investigated this possibility for running a lunar dynamo, and Ziegler and Stegman (2013) similarly sought an explanation for Earth's early magnetic field by this mechanism. Here, we apply the same methods to investigate whether a mantle dynamo is feasible for Mars.…”
Section: Introductionmentioning
confidence: 99%