Thermal Evolution and magnetic history of rocky planets

Abstract

We present a thermal evolution model coupled with a Henyey solver to study the circumstances under which a rocky planet could potentially host a dynamo in its liquid iron core and/or magma ocean. We calculate the evolution of planet thermal profiles by solving the energy balance equations for both the mantle and the core. We use a modified mixing length theory to model the convective heat flow in both the magma ocean and solid mantle. In addition, by including the Henyey solver, we self-consistently account for adjustments in the interior structure and heating (cooling) due to planet contraction (expansion). We evaluate whether a dynamo can operate using the critical magnetic Reynolds number. We run simulations to explore how planet mass ($M_{pl}$), core mass fraction (CMF) and equilibrium temperature ($T_{eq}$) affect the evolution and lifetime of possible dynamo sources. We find that the $T_{eq}$ determines the solidification regime of the magma ocean, and only layers with melt fraction greater than a critical value of 0.4 may contribute to the dynamo source region in the magma ocean. We find that the mantle mass, determined by $M_{pl}$ and CMF, controls the thermal isolating effect on the iron core. In addition, we show that the liquid core last longer with increasing planet mass. For a core thermal conductivity of 40$\mathrm{W}{\mathrm{m}}^{-1}{\mathrm{K}}^{-1}$, the lifetime of the dynamo in the iron core is limited by the lifetime of the liquid core for 1$M_{\oplus }$ planets, and by the lack of thermal convection for 3$M_{\oplus }$ planets.

arXiv comment33 pages, 16 figures. Submitted to ApJ

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• The Evolution of Jupiter and Saturn as a function of the Parameter R${}_{\rho }$
• Distribution of Europium in The Milky Way Disk; Its Connection to Planetary Habitability and The Source of The R-Process
• A Validated Low-to-Intermediate Mass Planetary Interior Structure Model and New Mass-Radius Relations