Observational constraint on the radius and oblateness of the lunar core-mantle boundary

Abstract

Lunar laser ranging (LLR) data and Apollo seismic data analyses, revealed independent evidence for the presence of a fluid lunar core. However, the size of the lunar fluid core remained uncertain by $\pm 55$ km (encompassing two contrasting 2011 Apollo seismic data analyses). Here we show that a new description of the lunar interior's dynamical model provides a determination of the radius and geometry of the lunar core-mantle boundary (CMB) from the LLR observations. We compare the present-day lunar core oblateness obtained from LLR analysis with the expected hydrostatic model values, over a range of previously expected CMB radii. The findings suggest a core oblateness ($f_c=(2.2\pm 0.6)\times 10^{-4}$) that satisfies the assumption of hydrostatic equilibrium over a tight range of lunar CMB radii (${\mathcal{R}}_{CMB}=381\pm 12$ km). Our estimates of a presently-relaxed lunar CMB translates to a core mass fraction in the range of $1.59-1.77\%$ with a present-day Free Core Nutation (FCN) within $(367\pm 100)$ years.

Accepted for publication in Geophysical Research Letters

References in corpus (2)

• Lunar Laser Ranging Tests of the Equivalence Principle
• An absolute calibration system for millimeter-accuracy APOLLO measurements

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