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The Atmosphere-Interior Connection: Rocky Planets As Linked Chemical

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The Atmosphere-Interior Connection: Rocky Planets As Linked Chemical Evolution of Rocky Planets Laura Schaefer Exoplanets in Our Backyard, Feb. 2020 Collaborators: Lindy Elkins-Tanton (ASU) Bruce Fegley (WashU) Edwin Kite (UChicago) Kaveh Pahlevan (SETI) Laura Kreidberg (CfA) Robin Wordsworth (Harvard) Dimitar Sasselov (CfA) Outline • Volatiles in rocky planet interiors • Atmosphere-magma ocean interaction • Deep volatile cycles Water in Earth’s Mantle Reference H2O in mantle (OM) Korenaga et al. 2017 0.56 – 1.3 Hirschmann (2018) 0.9 ± 0.2 Peslier et al. (2017) 1.1 - 7.4 Karato (2015) TGC Water in Earth’s Mantle Reference H2O in mantle (OM) Korenaga et al. 2017 0.56 – 1.3 Hirschmann (2018) 0.9 ± 0.2 Peslier et al. (2017) 1.1 - 7.4 Nestola & Smyth (2015) Bodnar et al. (2013) Peslier et al. (2017) Water on Venus and Mars McCubbin & Barnes (2019) Lecuyer et al. (2000) Peslier et al. 2019 Magma Oceans? • Earth: inferred from giant impact scenario for Moon formation • Lunar MO most robust • Venus: uncertain • Runaway greenhouse onset depends on uncertain stellar evolution • Core formation models (Jacobson et al. 2017) posit that Venus may not have experienced a late giant impact • Mars: rapid formation (~5-10 Myrs, Dauphas & Pourmand 2011) suggests at least a partial magma ocean • short-lived radionuclides and rapid accretion rate may be necessary (Saito & Kuramoto 2018) • Exoplanets: close-in planets, even M-dwarf habitable zone planets may experience extended runaway greenhouse driven magma oceans Type I Planets Type II Planets have oceans. lose their water. Hamano et al. (2013) Nature O2 uptake by magma ocean Mantles composed mostly of Mg, Si, Fe, and O Mg2+ MgO 4+ Si + n O2- = SiO2 Fe2+ FeO 3+ Fe Fe2O3 FeO(melt) + 0.5 O(g) = FeO1.5 (melt) Atmospheric O 10 M 2 1 M buildup • most sensitive to • Orbit • Albedo • Planet mass α = 0.7 100 bars CO2 Assumes no initial mantle Fe3+ and perfect uptake of O2 by mantle during magma ocean stage. Wordsworth et al. (2018) ApJ LHS 3844b – Atmosphere Detection?? Temperature Map Observations with the Spitzer Space Telescope The permanent dayside is 1200 degrees hotter than the nightside | 10 Figures from Kreidberg et al. (2019) Nature LHS 3844b – Atmosphere Stability to Erosion 10% Can constrain maximum initial planet water abundance and minimum stellar 1% heating Planet likely started with <2 wt% water 0.1% Earth has ~0.02 wt% water 0.01% Amount of initial water in the planet in initial of water Amount 10-4 10-3 10-2 High energy radiation fraction Thin atmospheres aren’t stable: LHS 3844b is a bare rocky planet Figures from Kreidberg et al. (2019) Nature | 11 Oxidation of Earth & Venus by atmosphere Oxidation of the mantle Loss of Water Venus 1.5 Earth Earth % FeO Wt Venus Radius of solidification (rs/Rp) Based on Schaefer et al. (2016), Wordsworth et al. (2018) Oxidation of Earth & Venus by atmosphere Loss of Water Earth Venus Lammer et al. (2018) Water loss and oxidation will depend on stellar evolution (fast vs. slow rotator) and timing Mars early magma ocean Lammer et al. (2018) Saito & Kuramoto (2018) Most magma ocean models miss some heat sources (e.g. gravitational segregation), that may enhance melt production Sub-Neptune “cores” are mostly molten Evolution of atmosphere- mantle temperature for planets with 4.5 MEarth “cores” and variable masses of H2 atmospheres Interiors of sub-Neptunes are mostly molten silicates Vazan et al. (2018) Large amounts of volatiles in “core” Reaction with FeO (8wt%) Reaction with Fe metal (50 wt%) Kite et al. (2020) ApJ, in revision H O + Fe (metal) = H + FeO H2 + FeO = Fe(metal) + H2O 2 2 Deep volatile cycles • Volcanic outgassing • Recycling of volatiles into mantle • Subduction of oceanic plates Plate tectonics • Plate delamination? Stagnant lid recycling? • Plume/Drip magmatism? Deep Water Cycle Karato (2015) TGC Water is transported into the mantle through subduction of hydrated minerals and sediments in a process called regassing or ingassing. Water escapes from the mantle through volcanic eruptions at mid-ocean ridges in a process called degassing or outgassing. Plate tectonics vs. Stagnant lid Kite et al. (2009) Kite Plate tectonics doesn’t operate on the hot Hadean and Archean Earth Plate tectonics may have started between 3.2-2.2 Gyr (Brown et al. 2020) Estimates of surface/mantle inventories suggest that most of Earth’s carbon is in the mantle, but most H2O and N is at the surface Based on current outgassing rates, the inventories require significant ingassing of C, but early large surface inventories of H and N Hirschmann (2018) Summary • A large portion of planetary volatile components are locked in planetary interiors • Initial solid mantle volatile abundances depend on solubilities, solid/melt partitioning, magma ocean lifetime and atmospheric escape • Deep volatile cycles depend on style of tectonics (PT vs. stagnant lid) • Earth has not always had plate tectonics • Stagnant lid planets have slower return of materials to interior • Exoplanets occupy a wider parameter space, so we have to ask, what are the limits in planet size/volatile content/etc that these models apply to?.
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