pub2018.bib

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@article{2018Icar..300..129M,
  author = {{Moore}, J.~M. and {Howard}, A.~D. and {Umurhan}, O.~M. and 
	{White}, O.~L. and {Schenk}, P.~M. and {Beyer}, R.~A. and {McKinnon}, W.~B. and 
	{Spencer}, J.~R. and {Singer}, K.~N. and {Grundy}, W.~M. and 
	{Earle}, A.~M. and {Schmitt}, B. and {Protopapa}, S. and {Nimmo}, F. and 
	{Cruikshank}, D.~P. and {Hinson}, D.~P. and {Young}, L.~A. and 
	{Stern}, S.~A. and {Weaver}, H.~A. and {Olkin}, C.~B. and {Ennico}, K. and 
	{Collins}, G. and {Bertrand}, T. and {Forget}, F. and {Scipioni}, F. and 
	{New Horizons Science Team}},
  title = {{Bladed Terrain on Pluto: Possible origins and evolution}},
  journal = {\icarus},
  keywords = {Pluto, Atmosphere, Ices, Mechanical properties, Geological processes, IR spectroscopy, Surface},
  year = 2018,
  volume = 300,
  pages = {129-144},
  abstract = {{Bladed Terrain on Pluto consists of deposits of massive CH$_{4}$,
which are observed to occur within latitudes 30{\deg} of the equator and
are found almost exclusively at the highest elevations ($\gt$ 2 km above
the mean radius). Our analysis indicates that these deposits of
CH$_{4}$ preferentially precipitate at low latitudes where net
annual solar energy input is lowest. CH$_{4}$ and N$_{2}$
will both precipitate at low elevations. However, since there is much
more N$_{2}$ in the atmosphere than CH$_{4}$, the
N$_{2}$ ice will dominate at these low elevations. At high
elevations the atmosphere is too warm for N$_{2}$ to precipitate
so only CH$_{4}$ can do so. We conclude that following the time of
massive CH$_{4}$ emplacement; there have been sufficient
excursions in Pluto's climate to partially erode these deposits via
sublimation into the blades we see today. Blades composed of massive
CH$_{4}$ ice implies that the mechanical behavior of
CH$_{4}$ can support at least several hundred meters of relief at
Pluto surface conditions. Bladed Terrain deposits may be widespread in
the low latitudes of the poorly seen sub-Charon hemisphere, based on
spectral observations. If these locations are indeed Bladed Terrain
deposits, they may mark heretofore unrecognized regions of high
elevation.
}},
  doi = {10.1016/j.icarus.2017.08.031},
  adsurl = {http://adsabs.harvard.edu/abs/2018Icar..300..129M},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}