Abstract
Context. Long-lived radioactive nuclides, such as 40K, 232Th, 235U, and 238U, contribute to persistent heat production in the mantle of terrestrial-type planets. As refractory elements, the concentrations of Th and U in a terrestrial exoplanet are implicitly reflected in the photospheric abundances of the stellar host. However, a robust determination of these stellar abundances is difficult in practice owing to the general paucity and weakness of the relevant spectral features. Aims. We draw attention to the refractory, r-process element europium, which may be used as a convenient and practical proxy for the population analysis of radiogenic heating in exoplanetary systems. Methods. As a case study, we present a determination of Eu abundances in the photospheres of α Cen A and B with high-resolution HARPS spectra and a strict line-by-line differential analysis. To first order, the measured Eu abundances can be converted into the abundances of 232Th, 235U, and 238U with observational constraints, while the abundance of 40K is approximated independently with a Galactic chemical evolution model. Results. Our determination shows that europium is depleted with respect to iron by ~0.1 dex and to silicon by ~0.15 dex compared to solar in the two binary components. The loci of α Cen AB at the low-ends of both [Eu/Fe] and [Eu/Si] distributions of a large sample of FGK stars further suggest significantly lower potential of radiogenic heat production in any putative terrestrial-like planet (i.e. α-Cen-Earth) in this system compared to that in rocky planets (including our own Earth) that formed around the majority of these Sun-like stars. Based on our calculations of the radionuclide concentrations in the mantle and assuming the mantle mass to be the same as that of our Earth, we find that the radiogenic heat budget in an α-Cen-Earth is 73.4−6.9+8.3 TW upon its formation and 8.8−1.3+1.7 TW at the present day, which is 23 ± 5% and 54 ± 5% lower than that in the Hadean Earth (94.9 ± 5.5 TW) and in the modern Earth (19.0 ± 1.1 TW), respectively. Conclusions. As a consequence, mantle convection in an α-Cen-Earth is expected to be overall weaker than that of Earth (assuming other conditions are the same), and thus such a planet would be less geologically active, suppressing its long-term potential to recycle its crust and volatiles. With Eu abundances being available for a large sample of Sun-like stars, the proposed approach can extend our ability to predict the nature of other rocky worlds that can be tested by future observations.
Highlights
A major goal of modern astronomy is to better define the nature of exoplanets and understand planet formation and evolution, as well as life prospects, in a cosmic perspective
To summarise our abundance analysis results, we find that europium is depleted with respect to iron in α Cen AB by ∼0.1 dex compared to the Sun and that there is a lack of evidence for a different Eu content in the two components
In the context of studying the potential of Eu as a convenient tool for diagnosing exoplanetary radiogenic heat power, we present a detailed determination of the abundances of this element in the photospheres of α Cen AB, our nearest Sun-like stars
Summary
A major goal of modern astronomy is to better define the nature of exoplanets and understand planet formation and evolution, as well as life prospects, in a cosmic perspective. To this end, communities in Earth sciences, exoplanet science, and stellar astrophysics have been increasingly joining forces through existing and future ground- and space-based astronomical infrastructures (e.g. Gaia, VLT, Kepler, TESS, ELT, JWST, PLATO) and/or collaboration networks (e.g. NExSS, PlanetS, GALAH). It is noteworthy that the heat-producing shortlived nuclides 26Al and 60Fe are important heating sources in shaping the composition of planetesimals in the early Solar System (Lichtenberg et al 2016) but become effectively extinct after ∼3 Myr and essentially do not contribute to heat production in already formed planets (Frank et al 2014)
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