Reorientation of Sputnik Planitia implies a subsurface ocean on Pluto

@article{Nimmo2016ReorientationOS,
  title={Reorientation of Sputnik Planitia implies a subsurface ocean on Pluto},
  author={Francis Nimmo and Douglas P. Hamilton and William B. McKinnon and Paul M. Schenk and Richard P. Binzel and Carver J. Bierson and Ross A. Beyer and J. M. Moore and S. Alan Stern and H. Weaver and Cathy B. Olkin and Leslie A. Young and K. Ennico Smith},
  journal={Nature},
  year={2016},
  volume={540},
  pages={94-96}
}
The deep nitrogen-covered basin on Pluto, informally named Sputnik Planitia, is located very close to the longitude of Pluto’s tidal axis and may be an impact feature, by analogy with other large basins in the Solar System. Reorientation of Sputnik Planitia arising from tidal and rotational torques can explain the basin’s present-day location, but requires the feature to be a positive gravity anomaly, despite its negative topography. Here we argue that if Sputnik Planitia did indeed form as a… 

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TLDR
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Planetary science: Pluto's telltale heart

TLDR
Modelling data suggest that Pluto's Sputnik Planitia basin may be an ice cap, rather than the product of an impact, and that the feature formed shortly after Pluto's largest satellite Charon did, and has since been stable.
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References

SHOWING 1-10 OF 38 REFERENCES

The rapid formation of Sputnik Planitia early in Pluto’s history

TLDR
Modelling suggests that Sputnik Planitia formed shortly after Charon did and has been stable, albeit gradually losing volume, over the age of the Solar System.

Reorientation and faulting of Pluto due to volatile loading within Sputnik Planitia

TLDR
It is reported that the location of Sputnik Planitia is the natural consequence of the sequestration of volatile ices within the basin and the resulting reorientation (true polar wander) of Pluto.

Formation of the Sputnik Planum basin and the thickness of Pluto's subsurface ocean

We simulate the formation of the large elliptical impact basin associated with Pluto's Sputnik Planum (SP; informal name). The location of SP suggests that it represents a large positive mass

Vigorous convection as the explanation for Pluto's polygonal terrain.

TLDR
A parameterized convection model is reported to compute the Rayleigh number of the N2 ice and show that it is vigorously convecting, making Rayleigh-Bénard convection the most likely explanation for these polygons on Pluto.

Convection in a volatile nitrogen-ice-rich layer drives Pluto's geological vigour.

TLDR
It is reported, on the basis of available rheological measurements, that solid layers of nitrogen ice with a thickness in excess of about one kilometre should undergo convection for estimated present-day heat-flow conditions on Pluto and shown numerically that convective overturn in a several-kilometre-thick layer of solid nitrogen can explain the great lateral width of the cells.

Recent tectonic activity on Pluto driven by phase changes in the ice shell

The New Horizons spacecraft has found evidence for geologic activity on the surface of Pluto, including extensional tectonic deformation of its water ice bedrock see Moore et al. (2016). One

Surface compositions across Pluto and Charon

TLDR
The New Horizons team presents the complex surface features and geology of Pluto and its large moon Charon, including evidence of tectonics, glacial flow, and possible cryovolcanoes, as well as their analysis of the encounter data downloaded so far.

Lunar Multiring Basins and the Cratering Process

Abstract Numerous studies of the lunar gravity field have concluded that the lunar Moho is substantially uplifted beneath the young multiring basins. This uplift is presumably due to the excavation

Climate zones on Pluto and Charon