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Large-scale cryovolcanic resurfacing on Pluto

Author

Listed:
  • Kelsi N. Singer

    (Southwest Research Institute)

  • Oliver L. White

    (Carl Sagan Center at the SETI Institute)

  • Bernard Schmitt

    (Université Grenoble Alpes, CNRS, IPAG)

  • Erika L. Rader

    (University of Idaho)

  • Silvia Protopapa

    (Southwest Research Institute)

  • William M. Grundy

    (Lowell Observatory)

  • Dale P. Cruikshank

    (Space Science Division)

  • Tanguy Bertrand

    (Space Science Division
    University Pierre et Marie Curie, University Paris-Diderot)

  • Paul M. Schenk

    (Lunar and Planetary Institute)

  • William B. McKinnon

    (Washington University)

  • S. Alan Stern

    (Southwest Research Institute)

  • Rajani D. Dhingra

    (California Institute of Technology)

  • Kirby D. Runyon

    (Johns Hopkins University Applied Physics Laboratory)

  • Ross A. Beyer

    (Carl Sagan Center at the SETI Institute)

  • Veronica J. Bray

    (University of Arizona)

  • Cristina Dalle Ore

    (Carl Sagan Center at the SETI Institute)

  • John R. Spencer

    (Southwest Research Institute)

  • Jeffrey M. Moore

    (Space Science Division)

  • Francis Nimmo

    (University of California)

  • James T. Keane

    (California Institute of Technology)

  • Leslie A. Young

    (Southwest Research Institute)

  • Catherine B. Olkin

    (Southwest Research Institute)

  • Tod R. Lauer

    (National Science Foundation National Optical Infrared Astronomy Research Laboratory)

  • Harold A. Weaver

    (Johns Hopkins University Applied Physics Laboratory)

  • Kimberly Ennico-Smith

    (Space Science Division)

Abstract

The New Horizons spacecraft returned images and compositional data showing that terrains on Pluto span a variety of ages, ranging from relatively ancient, heavily cratered areas to very young surfaces with few-to-no impact craters. One of the regions with very few impact craters is dominated by enormous rises with hummocky flanks. Similar features do not exist anywhere else in the imaged solar system. Here we analyze the geomorphology and composition of the features and conclude this region was resurfaced by cryovolcanic processes, of a type and scale so far unique to Pluto. Creation of this terrain requires multiple eruption sites and a large volume of material (>104 km3) to form what we propose are multiple, several-km-high domes, some of which merge to form more complex planforms. The existence of these massive features suggests Pluto’s interior structure and evolution allows for either enhanced retention of heat or more heat overall than was anticipated before New Horizons, which permitted mobilization of water-ice-rich materials late in Pluto’s history.

Suggested Citation

  • Kelsi N. Singer & Oliver L. White & Bernard Schmitt & Erika L. Rader & Silvia Protopapa & William M. Grundy & Dale P. Cruikshank & Tanguy Bertrand & Paul M. Schenk & William B. McKinnon & S. Alan Ster, 2022. "Large-scale cryovolcanic resurfacing on Pluto," Nature Communications, Nature, vol. 13(1), pages 1-9, December.
    • Handle: RePEc:nat:natcom:v:13:y:2022:i:1:d:10.1038_s41467-022-29056-3
    DOI: 10.1038/s41467-022-29056-3
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    References listed on IDEAS

    as
    1. Tanguy Bertrand & François Forget, 2016. "Observed glacier and volatile distribution on Pluto from atmosphere–topography processes," Nature, Nature, vol. 540(7631), pages 86-89, December.
    2. Tanguy Bertrand & François Forget & Bernard Schmitt & Oliver L. White & William M. Grundy, 2020. "Equatorial mountains on Pluto are covered by methane frosts resulting from a unique atmospheric process," Nature Communications, Nature, vol. 11(1), pages 1-7, December.
    3. John E. Moores & Christina L. Smith & Anthony D. Toigo & Scott D. Guzewich, 2017. "Penitentes as the origin of the bladed terrain of Tartarus Dorsa on Pluto," Nature, Nature, vol. 541(7636), pages 188-190, January.
    Full references (including those not matched with items on IDEAS)

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