Planetary thermal evolution models with tectonic transitions

TL;DR

This paper develops advanced numerical models for planetary thermal evolution that incorporate complex interior rheologies and tectonic transitions, providing new insights into heat transfer dynamics and their implications for planetary evolution.

Contribution

It introduces a novel approach to modeling planetary interiors with complex rheologies and tectonic transitions, generating statistically-based Nu-Ra scalings that account for various physical effects.

Findings

Nu-Ra exponent ~0.26 for mobile lid systems

Nu-Ra exponent ~0.12 for stagnant-lid systems

Time lag of 200-300 Myr between Ra and Nu

Abstract

Thermal history calculations provide important insights into the interior evolution of planets, but incorporate simplified dynamics from the systems they represent. Planetary interiors typical incorporate complex rheologies, viscous layering, lateral heterogeneities, and time delays in processes, which have not been traditionally represented by parameterised approaches. Here we develop numerical models for planetary evolution, incorporating the physical complexity of Earth's interior, and use them to generate statistically-based Nu-Ra scalings. These encapsulate the main effects of tectonic transitions, geometry, and depth-dependent rheology, and time-sensitivity. We find an exponent $\beta$ of ~0.26 best describes the Nu-Ra relationship for evolving mobile lid systems, and $\beta$ ~0.12 for stagnant-lid systems. Systems with time dependent subduction have $\beta$ varying between ~0.26 during the Hadean, when external factors such as impacts facilitate tectonics, to ~0.12 during the Archaean, when the system is dominated by long periods of quiescence, and systems driven by external forcings (eg. due to impacts in the first 100Myr of Earth's history) may exhibit much higher exponents. We also find a time-lag between Ra (which primarily depends on mantle temperature) and Nu (normalised surface heat flow) of around 200-300Myr, suggesting a significant delay between mantle thermal configuration, and its surface manifestation. These results provide an approach for the rapid characterisation of tectonic, volcanic, and atmospheric evolution of terrestrial exoplanets.