TY - JOUR
T1 - Habitability of Exoplanet Waterworlds
AU - Kite, Edwin S.
AU - Ford, Eric B.
N1 - Funding Information:
We are grateful to Bruce Fegley for continuing guidance on geochemical thermodynamics. We thank Norm Sleep for a stimulating and prompt formal review, which improved the manuscript. We thank Christophe Cossou, Itay Halevy, Jim Kasting, Ravi Kumar Kopparapu, Nataly Ozak, and Ramses Ramirez, for unselfish sharing of research output. We thank Dorian Abbot, Jonathan Lunine, Nadejda Marounina, Marc Neveu, and Ramses Ramirez for commenting on a draft. We thank David Archer, Paul Asimow, Fred Ciesla, Eric Fiegelson, Jim Fuller, Eric Gaidos, Marc Hirschmann, Manasvi Lingam, Mohit Melwani Daswani, Jack Mustard, Leslie Rogers, Laura Schaefer, Hilke Schlichting, Norm Sleep, Sarah Stewart, Cayman Unterborn, and Steve Vance, who each provided useful advice. We thank the CHIM-XPT team: Mark Reed, Nicolas Spycher, and Jim Palandri. We thank Craig Manning and Tim Lichtenberg for sharing preprints. We thank the organizers of the University of Michigan volatile origins workshop. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Parts of this research were conducted with Advanced CyberInfrastructure computational resources provided by The Institute for CyberScience at The Pennsylvania State University (http://ics.psu.edu), including the CyberLAMP cluster supported by NSF grant MRI-1626251. The results reported herein benefitted from collaborations and/or information exchange within NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate. This work was supported by the U.S. taxpayer, primarily via NASA grant NNX16AB44G.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved..
PY - 2018/9/1
Y1 - 2018/9/1
N2 - Many habitable zone (HZ) exoplanets are expected to form with water mass fractions higher than that of the Earth. For rocky exoplanets with 10-1000× Earth's H2O but without H2, we model the multi-Gyr evolution of ocean temperature and chemistry, taking into account C partitioning, high-pressure ice phases, and atmosphere-lithosphere exchange. Within our model, for Sun-like stars, we find that: (1) the duration of habitable surface water is strongly affected by ocean chemistry; (2) possible ocean pH spans a wide range; (3) surprisingly, many waterworlds retain habitable surface water for >1 Gyr, and (contrary to previous claims) this longevity does not necessarily involve geochemical cycling. The key to this cycle-independent planetary habitability is that C exchange between the convecting mantle and the water ocean is curtailed by seafloor pressure on waterworlds, so the planet is stuck with the ocean mass and ocean cations that it acquires during the first 1% of its history. In our model, the sum of positive charges leached from the planetary crust by early water-rock interactions is-coincidentally-often within an order of magnitude of the early-acquired atmosphere+ocean inorganic C inventory overlaps. As a result, p CO2 is frequently in the "sweet spot" (0.2-20 bar) for which the range of semimajor axis that permits surface liquid water is about as wide as it can be. Because the width of the HZ in the semimajor axis defines (for Sun-like stars) the maximum possible time span of surface habitability, this effect allows for Gyr of habitability as the star brightens. We illustrate our findings by using the output of an ensemble of N-body simulations as input to our waterworld evolution code. Thus (for the first time in an end-to-end calculation) we show that chance variation of initial conditions, with no need for geochemical cycling, can yield multi-Gyr surface habitability on waterworlds.
AB - Many habitable zone (HZ) exoplanets are expected to form with water mass fractions higher than that of the Earth. For rocky exoplanets with 10-1000× Earth's H2O but without H2, we model the multi-Gyr evolution of ocean temperature and chemistry, taking into account C partitioning, high-pressure ice phases, and atmosphere-lithosphere exchange. Within our model, for Sun-like stars, we find that: (1) the duration of habitable surface water is strongly affected by ocean chemistry; (2) possible ocean pH spans a wide range; (3) surprisingly, many waterworlds retain habitable surface water for >1 Gyr, and (contrary to previous claims) this longevity does not necessarily involve geochemical cycling. The key to this cycle-independent planetary habitability is that C exchange between the convecting mantle and the water ocean is curtailed by seafloor pressure on waterworlds, so the planet is stuck with the ocean mass and ocean cations that it acquires during the first 1% of its history. In our model, the sum of positive charges leached from the planetary crust by early water-rock interactions is-coincidentally-often within an order of magnitude of the early-acquired atmosphere+ocean inorganic C inventory overlaps. As a result, p CO2 is frequently in the "sweet spot" (0.2-20 bar) for which the range of semimajor axis that permits surface liquid water is about as wide as it can be. Because the width of the HZ in the semimajor axis defines (for Sun-like stars) the maximum possible time span of surface habitability, this effect allows for Gyr of habitability as the star brightens. We illustrate our findings by using the output of an ensemble of N-body simulations as input to our waterworld evolution code. Thus (for the first time in an end-to-end calculation) we show that chance variation of initial conditions, with no need for geochemical cycling, can yield multi-Gyr surface habitability on waterworlds.
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U2 - 10.3847/1538-4357/aad6e0
DO - 10.3847/1538-4357/aad6e0
M3 - Article
AN - SCOPUS:85053154945
SN - 0004-637X
VL - 864
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 75
ER -