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Title: Radiogenic Heating and its Influence on Rocky Planet Dynamos and Habitability
Authors: Francis Nimmo et al.
First Author’s Institution: University of California Santa Cruz
Status: Published in ApJL
Rocky planets are thought to start as hot masses of material accreting from a disk of gas and dust around their young host star. Whereas the primary heat source early on comes from accretion, and orbital dynamics can lead to further heating through tidal squeezing, the ongoing thermal evolution of many rocky planets is likely controlled by radiogenic heat production. In particular, the radioactive isotopes of uranium (U) and thorium (Th) have long half-lives and so may be significant in deciding the long-term geodynamic history. The authors of today’s bite argue that the exact concentrations of such elements in a planet’s mantle could decide the presence and strength of that world’s magnetic field.
Dynamo theory holds that magnetic fields are generated by circulation of conductive fluids. In the case of Earth, convection of hot liquid metals in the outer core may be generating our magnetic field (see Figure 1). This outer core dynamo shuffles heat outward from the planet’s interior and its efficiency is controlled by the temperature of the overlying mantle. Thus, our magnetic field can be linked to heat production in the mantle that is mainly due to the decay of radiogenic elements. But what would it mean if our planet happened to have more or less of these elements?
Figure 1: Simplified cross-section of the common interpretation for Earth’s interior. The thin layer at the Earth’s surface is the crust (brown), below that is the mantle (red), which extracts heat from the liquid outer core (yellow), which convects to produce the magnetic field and gradually solidifies to form the inner core (white). [universe-review.ca]
The models at the center of today’s paper are relatively simple compared to more computationally expensive 2D or 3D models, but are sufficient to see how changing a parameter like mantle heat production could affect a planet’s evolution. They consider the timeline of three identical Earths, where the only difference is having less U and Th (Figure 2a), Earth-like concentrations (Figure 2b), or more U and Th (Figure 2c). All cases assume that plate tectonics contributes to heat transfer, because previous work suggests magnetic dynamos are more likely under conditions conducive to plate tectonics, despite its presence not being a certainty (see Venus, for example). In Figure 2, the authors use entropy production as a proxy for the likelihood and intensity of a dynamo. The entropy production rate determines the presence of a dynamo based on whether it exceeds the adiabatic entropy rate, where the adiabat defines the expected temperature and pressure conditions for the mantle. Dynamo convection is at first due to extraction of heat into the mantle that gradually declines, but rapidly increases again after the core cools enough to begin solidifying. This extra burst of activity is due to “compositional buoyancy” where solidification of the core releases light elements into the fluid above.
As a good starting point, the trend predicted by the model for normal Earth (Figure 2b) matches geologic observations that the Earth has had an active magnetic field for over 3.5 billion years, though it turned off or weakened at least once for a few million years. In fact, it seems that Earth was just on the threshold for having a consistently active dynamo, based on how the entropy production may have briefly dipped below the threshold around one billion years ago. In the case of less radiogenic heat than normal Earth (Figure 2a), solid core formation starts earlier and the dynamo is easily maintained. In the case of more radiogenic heat (Figure 2c), the dynamo may turn off for hundreds of millions of years because a high-temperature mantle isn’t as effective at extracting heat from the core. So, opposite to what you might expect, the authors find that more radiogenic heat in the mantle leads to less core heat flux, less dynamo, and a smaller solid core.
Figure 2: Model results for (a) 0.33, (b) 1, and (c) 3 times Earth’s U and Th concentrations. The upper panels show decreasing heat flow over time (solid lines) and the onset of inner core formation (dashed green line). The lower panels show the entropy production rate over time, which generally decreases until inner core formation begins. The dynamo is thought to operate only when the total entropy rate (black) is greater than the adiabatic entropy rate (red). [Nimmo et al. 2020]
Figure 3: Rate of entropy production (indicated by color) for a varying fraction of radiogenic elements compared to normal Earth (in log scale) over time. Solid black lines indicate a reference temperature and the dashed red lines show the trajectory of three modeled scenarios through time (the author’s Figure 1 is referenced as Figure 2 in this astrobite). Note the black region where too much radiogenic heat kills the dynamo. [Nimmo et al. 2020]
Original astrobite edited by Spencer Wallace.
About the author, Anthony Maue:
Anthony is a PhD student at Northern Arizona University in Flagstaff studying planetary geology. In particular, his research focuses on Titan’s fluvial processes through analyses of Cassini radar data, laboratory experiments, and terrestrial field analog studies. Outside of school, Anthony enjoys skiing, cycling, running, music and film.