Tidal Heating of the Lunar Magma Ocean: Reconciling an Old Moon with a Young Solidification

TL;DR

This paper proposes that tidal heating within the lunar magma ocean explains the young lunar sample ages and suggests a long-lived molten state, reconciling an old Moon with the observed crystallization timeline.

Contribution

It introduces a model where tidal heating significantly influences lunar magma ocean evolution, explaining the young ages and lunar dichotomy.

Findings

Tidal heating offsets early heat loss, maintaining a molten state for over 150 million years.

The final solidification occurred rapidly near 4.35 Ga, explaining the age cluster.

Predicted asymmetric crystallization may account for lunar nearside-farside differences.

Abstract

The timing of the Moon's formation is fundamental to understanding the early Earth-Moon system. Ages of lunar magma ocean (LMO) crystallization have long been regarded as a key proxy for that event. Yet returned lunar sample ages cluster near the relatively young age of ~4.35 billion years ago (Ga). These ages are commonly interpreted as recording either a young-Moon formation age or later thermal resetting. Here we show that, for an old Moon (>4.5 Ga), the ~4.35 Ga age cluster can instead arise naturally from early LMO thermal evolution under Earth's tidal forcing. We identify tidal heating within a partially molten LMO as a major internal heat source. It offsets much of the early heat loss and maintains a long-lived high-energy state for >150 million years. As crystallization proceeded, this stable state was ultimately lost through the rapid collapse of tidal heating. The last stages of LMO solidification were compressed into a short interval near ~4.35 Ga. The tidal heat source decouples Moon formation from final LMO solidification. As an outcome of LMO evolution, we predict asymmetric late-stage crystallization between the lunar nearside and farside, potentially linking tidally modulated LMO evolution to the long-term lunar dichotomy.