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Investigating the atmospheric evolution of habitable worlds with a coupled climate-interior-redox model

Presentation #0201 in the session “Identifying Biosignatures”.

Published onMar 17, 2021
Investigating the atmospheric evolution of habitable worlds with a coupled climate-interior-redox model
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The atmospheric evolution of terrestrial planets is sculped by a range of complex astrophysical, geophysical, and geochemical processes. Interpreting observations of ostensibly habitable exoplanets will require an improved understanding of how these competing influences interact on long timescales. In particular, the interpretation of potential biosignature gases, such as oxygen, is contingent upon understanding the probable redox evolution of lifeless worlds. Here, we develop a generalized model of terrestrial planet atmospheric evolution to anticipate observations of habitable exoplanets. The model, which is shown schematically in Fig. 1, connects early magma ocean evolution to subsequent, temperate geochemical cycling. The thermal evolution of the interior, cycling of C-H-O bearing volatiles, surface climate, crustal production, and atmospheric escape are explicitly coupled throughout this evolution. The redox evolution of the atmosphere is controlled by net planetary oxidation via the escape of H to space, the loss of atmospheric oxygen to the magma ocean, and oxygen consumption via crustal sinks such as outgassing of reduced species, serpentinization reactions, and direct “dry” oxidation of fresh crust.

The model can successfully reproduce the atmospheric evolution of a lifeless Earth: it consistently predicts an anoxic atmosphere and temperate surface conditions after 4.5 Gyrs of evolution. This result is insensitive to model uncertainties such as the details of atmospheric escape, mantle convection parameterizations, initial radiogenic inventories, the efficiency of crustal oxygen sinks, and unknown carbon cycle and deep-water cycle parameters. This suggests abundant oxygen is a reliable biosignature for literal Earth twins, defined as Earth-sized planets at 1 AU around sunlike stars with 1-10 Earth oceans and less initial carbon dioxide than water.

However, if initial volatile inventories are permitted to vary outside these “Earth-like” ranges, then dramatically different redox evolution trajectories are permitted. We identify three scenarios whereby Earth-sized planets in the habitable zones of sunlike stars could accumulate oxygen rich atmospheres (0.01–1 bar) in the absence of life. Specifically, (i) high initial CO2:H2O endowments, (ii), >50 Earth ocean water inventories, or (iii) extremely volatile poor initial inventories, could all result in oxygen-rich atmospheres after 4.5 Gyrs of evolution. These false positives arise despite the assumption that there is always sufficient non-condensible atmospheric gases, N2, to maintain an effective cold trap (Wordsworth & Pierrehumbert 2014). Fortunately, all three of these oxygen false positive scenarios could potentially be identified by thorough characterization of the planetary context. Using time resolved photometry to deduce surface maps would be especially helpful in ruling out high water inventory, waterworld false positives (Lustig-Yaeger et al. 2018).

The model also sheds light on the atmospheric evolution of Venus and Venus-like exoplanets. We can successfully recover the modern state of Venus’ atmosphere, including a dense CO2-dominated atmosphere with negligible water vapor and molecular oxygen. Moreover, there is a clear dichotomy in the evolutionary scenarios that recover modern Venus conditions, one in which Venus was never habitable and perpetually in runaway greenhouse since formation, and another whereby Venus experienced ~1-2 Gyr of surface habitability with a ~100 m deep ocean (c.f. Way et al. 2016). We explore the likelihood of each scenario and suggest future in situ observations that could help discriminate between these two alternative histories.

Figure 1

Schematic of terrestrial planet geochemical evolution model. The planetary redox budget, thermal-climate evolution, and volatile budget are modeled from initial magma ocean (left) through to temperate geochemical cycling (right). Oxygen fluxes are shown by green arrows, energy fluxes by black arrows, carbon fluxes by orange arrows, and water fluxes by blue arrows. Note that the net loss of H to space effectively adds oxygen to the atmosphere. During the magma ocean phase, the radius of solidification, rs, begins at the core-mantle boundary and moves toward the surface as internal heat is dissipated. The rate at which this occurs is controlled by radiogenic heat production, Qradioactive, and convective heatflow from the mantle to the surface, qm. This internal heatflow balances the difference between outgoing longwave radiation, OLR, and incoming shortwave radiation, ASR. The oxygen fugacity of the mantle, fO2, and the water and carbon content mantle and surface reservoirs are tracked throughout.

References

  • Lustig-Yaeger, J., et al. (2018). Detecting ocean glint on exoplanets using multiphase mapping. The Astronomical Journal, 156(6), 301.

  • Way, M. J., et al. (2016). Was Venus the first habitable world of our solar system? Geophysical Research Letters, 43(16), 8376-8383.

  • Wordsworth, R., & Pierrehumbert, R. (2014). Abiotic oxygen-dominated atmospheres on terrestrial habitable zone planets. The Astrophysical Journal Letters, 785(2), L20.

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