geology of Pluto

{{see also|Geography of Pluto}}

File:Pluto by LORRI, 11 July 2015.jpg

More than 98 percent of Pluto's surface consists of solid nitrogen, with traces of methane and carbon monoxide. The face of Pluto oriented toward Charon contains more solid methane,{{cite web |last= Lewin |first= Sarah |title= Pluto's 'Skyscrapers': What's Responsible for Dwarf Planet's Giant Ice Blades |url= https://www.space.com/38281-pluto-giant-ice-blades-explained.html |date= 27 September 2017 |work= Space.com |access-date= 27 September 2017 }} whereas the opposite face contains more nitrogen and solid carbon monoxide. Distribution of volatile ices is thought to be season-dependent and influenced more by solar insolation and topography than by subsurface processes.{{cite journal |last1=Bertrand |first1=Tanguy |last2=Forget |first2=François |s2cid=4401893 |title=Observed glacier and volatile distribution on Pluto from atmosphere–topography processes |journal=Nature |date=19 September 2016 |volume=540 |issue=7631 |pages=86–89 |doi=10.1038/nature19337 |pmid=27629517 |bibcode= 2016Natur.540...86B }}

Maps produced from images taken by the Hubble Space Telescope (HST), together with Pluto's light curve and the periodic variations in its infrared spectra, indicate that Pluto's surface is very varied, with large differences in both brightness and color, with albedos between 0.49 and 0.66. Pluto is one of the most contrastive bodies in the Solar System, with as much contrast as Saturn's moon Iapetus. The color varies between charcoal black, dark orange and white. New Horizons data suggest equally variable surface ages for Pluto, with ancient, dark, mountainous terrain occurring alongside the bright, flat, effectively craterless Sputnik Planitia and various terrains of intermediate age and color.

Pluto's surface color changed between 1994 and 2003: the northern polar region brightened and the southern hemisphere darkened. Pluto's overall redness also increased substantially between 2000 and 2002. These rapid changes probably relate to seasonal condensation and sublimation of portions of Pluto's atmosphere, amplified by Pluto's extreme axial tilt and high orbital eccentricity.

Pluto-Map-Annotated.jpg|The portions of Pluto's surface mapped by New Horizons. Center is 180 degrees longitude (diametrically opposite the moon Charon).

PIA20154-Pluto-MapOfOver1000Craters-20151110.jpg|Distribution of over 1000 craters of all ages on Pluto. The variation in density indicates a long history of varying geological activity.

Pluto's Sputnik Planum geologic map (cropped).jpg|Geologic map of Sputnik Planitia and surroundings (context), with convection cell margins outlined in black

Sputnik Planitia appears to be composed of ices more volatile, softer and more dense than the water-ice bedrock of Pluto, including nitrogen, carbon monoxide and solid methane.{{cite web

| url = http://www.planetary.org/blogs/emily-lakdawalla/2015/12211538-pluto-updates-from-agu.html

| title = Pluto updates from AGU and DPS: Pretty pictures from a confusing world

| last = Lakdawalla | first = Emily | author-link=Emily Lakdawalla | date =2015-12-21

| publisher = The Planetary Society | access-date = 2016-01-24}} A polygonal convection cell structure is visible over much of the planitia. No craters have been found, indicating that its surface must be less than 10 million years old.{{cite journal|last1= Marchis|first1= F.|last2= Trilling|first2= D. E.|title= The Surface Age of Sputnik Planum, Pluto, Must Be Less than 10 Million Years|journal= PLOS ONE|volume= 11|issue= 1 |date= 2016-01-20 |pages= e0147386 |doi= 10.1371/journal.pone.0147386 |arxiv = 1601.02833 | bibcode = 2016PLoSO..1147386T|pmid= 26790001|pmc= 4720356|doi-access= free}} A number of mechanisms are proposed to explain the absence of craters, including cryovolcanism (volcanoes erupting volatiles instead of magma), convective overturn, and viscous relaxation – processes that would erase negative topography. Glaciers of what is probably solid nitrogen can be seen flowing from the planitia into adjacent depressions and craters. Nitrogen from the plain appears to have been carried via the atmosphere and deposited in a thin layer of ice on uplands to the east and south of the plain, forming the large bright eastern lobe of Tombaugh Regio. Glaciers appear to be flowing back into the planitia through valleys from these eastern highlands.

{{multiple image |caption_align=center |align= center | width= |direction= horizontal

|header=

|image1=NH-Pluto-FrozenCarbonMonoxide-20150714.jpg

|caption1=Localization of frozen carbon monoxide in Sputnik Planitia (shorter contours represent higher concentrations).

|width1= 300

|image2= Troughs in Sputnik Planum by LORRI - crop of PIA19936.jpg

|caption2= Polygonal ice patterns in southern Sputnik Planitia (context) due to convection. Dark spots in the troughs at lower left are pits.{{cite news |last= Chang |first= Kenneth |title= Pluto terrain yields big surprises in New Horizons images |url= https://www.nytimes.com/2015/07/18/science/space/pluto-terrain-yields-big-surprises-in-new-horizons-images.html |date= 17 July 2015 |work= The New York Times |access-date= 17 July 2015 }}

|width2= 170

|image3= Pluto-puzzling-pits-2.png

|caption3= Closeup view of sublimation pits (context) in Sputnik Planitia

|width3= 114

|image4= PIA20151-Pluto-PitsInSputnikPlanum-20151110.jpg

|caption4= Additional views of Sputnik Planitia sublimation pits (context); some (left image) have dark material within

|width4=250

}}

{{Gallery| align=center |width=210

|File:Flowing nitrogen ice on Pluto.jpg| The northern edge of Sputnik Planitia (context), with indications of nitrogen ice flowing into and filling adjacent depressions.

|File:Nh-3flow-detail-annotated-9-17-15.jpg| Nitrogen ice glaciers flow from uplands through valleys into east Sputnik Planitia (context). Arrows indicate valley sides (which are 3 to 8 km apart) and the flow front in the planitia.

|File:PIA19943 - Intricate Valley Glaciers in Sputnik Planum, annotated.jpg| Nitrogen ice glaciers flowing into the eastern margin of the planitia (similar reprojected backlit view highlighting flow lines).

}}

Mountains several kilometres high occur along the southwestern and southern edges of Sputnik Planitia. Water ice is the only ice detected on Pluto that is strong enough at Plutonian temperatures to support such heights.

{{Gallery|align=center |width=210

|File:PIA20374-Pluto-NewHorizons-WaterIce-20150714.jpg|Pluto - water ice distribution (false color; rel 29 January 2016)

|File:NH-Pluto-WaterIceDetected-BlueRegions-Released-20151008.jpg| Regions where water ice has been detected (blue regions)

|File:NH-Pluto-SputnikPlanum-HillaryMontes-NorgayMontes-20150714.jpg| Hillary Montes and Tenzing Montes (labeled Norgay Montes) lie between Sputnik Planitia (top) and Belton Regio (bottom).{{cite web |last= Gipson |first= Lillian |title= New Horizons Discovers Flowing Ices on Pluto |url= http://www.nasa.gov/feature/new-horizons-discovers-flowing-ices-on-pluto |date= 24 July 2015 |work= NASA |access-date= 24 July 2015 |archive-date= 17 March 2016 |archive-url= https://web.archive.org/web/20160317050557/http://www.nasa.gov/feature/new-horizons-discovers-flowing-ices-on-pluto/ |url-status= dead }}

}}

Belton Regio and other dark areas have many craters and signatures of solid methane. The dark red color is thought to be due to tholins falling out of Pluto's atmosphere.

The mid-northern latitudes display a variety of terrain reminiscent of the surface of Triton. A polar cap consisting of solid methane "diluted in a thick, transparent slab of solid nitrogen" is somewhat darker and redder.{{cite web | title = Solar System Exploration: Multimedia: Gallery: Planetary Images: Pluto: The Ice Plot Thickens | publisher = NASA | url = http://solarsystem.nasa.gov/multimedia/display.cfm?Category=Planets&IM_ID=20257 | access-date = 2015-08-11 | archive-url = https://web.archive.org/web/20150818092817/http://solarsystem.nasa.gov/multimedia/display.cfm?Category=Planets&IM_ID=20257 | archive-date = 18 August 2015 | url-status = dead }}

{{Gallery|align= center |width= 210

|File:NH-Pluto-MethaneIce-20150715.png| Distribution of methane ice on Pluto. Bright green is the polar cap; bright red is Harrington Regio.

|File:NH-Pluto-MethaneIce-20150924.jpg| Map of methane ice abundance, which shows striking regional differences. Stronger methane absorption indicated by the brighter purple colors here, and lower abundances shown in black.

|File:NH-07-10-15-Pluto-FirstGeology-20150709.jpg| Indications of complex geological features north of the dark equatorial regions

}}

File:Snakeskin terrain covering Tartarus Dorsa.png

The western part of Pluto's northern hemisphere consists of an extensive, highly distinctive set of 500-meter-high mountains informally named Tartarus Dorsa; the spacing and shape of the mountains looks similar to scales or to tree bark. A January 2017 Nature paper by Dr. John Moores and his colleagues identified these icy ridges as penitentes.{{cite journal|last1= Moores|first1= John E.|last2= Smith|first2= Christina L.|last3= Toigo|first3= Anthony D.|last4= Guzewich|first4= Scott D.|title= Penitentes as the origin of the bladed terrain of Tartarus Dorsa on Pluto|journal= Nature|date= 4 January 2017|volume= 541|issue= 7636|pages= 188–190|doi= 10.1038/nature20779|pmid= 28052055 |arxiv = 1707.06670 | bibcode = 2017Natur.541..188M |s2cid= 4388677}} Penitentes are icy depressions formed by erosion and surrounded by tall spires. Pluto is the only planetary body other than Earth on which penitentes have been identified. Although penitentes have been hypothesized on Jupiter's satellite Europa, current theories suggest they may require an atmosphere to form. Moores and his colleagues hypothesize that Pluto's penitentes grow only during periods of high atmospheric pressure, at a rate of approximately 1 centimeter per orbital cycle. These penitentes appear to have formed in the last few tens-of-millions of years, an idea supported by the sparsity of craters in the region, making Tartarus Dorsa one of the youngest regions on Pluto.

Cutting through both Tartarus Dorsa and Pluto's heavily cratered northern terrain (and thus formed more recently than both) is a set of six canyons radiating from a single point; the longest, informally named Sleipnir Fossa, is over 580 kilometers long. These chasms are thought to have originated from pressures caused by material upwelling at the center of the formation.{{cite web|editor-last= Talbert|editor-first= Tricia|url= http://www.nasa.gov/feature/icy-spider-on-pluto|title= Icy 'Spider' on Pluto|publisher= NASA|date= 8 April 2016|access-date= 23 February 2017|archive-date= 21 March 2023|archive-url= https://web.archive.org/web/20230321173403/https://www.nasa.gov/feature/icy-spider-on-pluto/|url-status= dead}}

When New Horizons first sent back data from Pluto, Pluto was thought{{by whom|date=April 2019}} to be losing hundreds of tons of its atmosphere an hour to ultraviolet light from the Sun; such an escape rate would be too great to be resupplied by comet impacts. Instead, nitrogen was thought to be resupplied either by cryovolcanism or by geysers bringing it to the surface. Images of structures that imply upwelling of material from within Pluto, and streaks possibly left by geysers, support this view.{{cite web | title= Scientists study nitrogen provision for Pluto's atmosphere| publisher= phys.org| date= 2015-08-11|url= http://phys.org/news/2015-08-scientists-nitrogen-provision-pluto-atmosphere.html |access-date= 11 August 2015}} Subsequent discoveries suggest that Pluto's atmospheric escape was overestimated by several thousand times and thus Pluto could theoretically keep its atmosphere without geological assistance, though evidence of ongoing geology remains strong.{{Cite web | url= http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20151109 | title= New Horizons: News Article?page=20151109}}

Two possible cryovolcanoes, Wright Mons and Piccard Mons, have been identified in topographic maps of the region south of Sputnik Planitia, near the south pole. Both are over 150 km across and at least 4 km high, the tallest peaks known on Pluto at present. They are lightly cratered and thus geologically young, although not as young as Sputnik Planitia. They are characterized by a large summit depression and hummocky flanks. This represents the first time large potentially cryovolcanic constructs have been clearly imaged anywhere in the Solar System.{{cite web

| url = http://pluto.jhuapl.edu/News-Center/News-Article.php?page=20151109

| title = At Pluto, New Horizons Finds Geology of All Ages, Possible Ice Volcanoes, Insight into Planetary Origins

| date = 2015-11-09 | website = New Horizons News Center

| publisher = The Johns Hopkins University Applied Physics Laboratory LLC

| access-date = 2015-11-09}}{{cite journal

| url = http://www.nature.com/news/icy-volcanoes-may-dot-pluto-s-surface-1.18756

| title = Icy volcanoes may dot Pluto's surface

| last = Witze | first = A. | date = 2015-11-09 | journal = Nature

| access-date = 2015-11-09 | doi = 10.1038/nature.2015.18756

| s2cid = 182698872

}}{{cite web

| url = http://www.space.com/31073-pluto-ice-volcano-mountains-photos.html

| title = Icy Volcanoes May Erupt on Pluto | last = Redd | first = N. T. | date = 2015-11-09 | publisher = Space.Com

| access-date = 2015-11-10}}

A 2019 study identified a second likely cryovolcanic structure around Virgil Fossae, a series of troughs in northeastern Belton Regio, west of Tombaugh Regio. Ammonia-rich cryolavas appear to have erupted from Virgil Fossae and several nearby sites and covered an area of several thousand square kilometers; the fact that the ammonia's spectral signal was detectable when New Horizons flew by Pluto suggests that Virgil Fossae is no older than one billion years and potentially far younger, as galactic cosmic rays would destroy all the ammonia in the upper meter of the crust in that time and solar radiation could destroy the surface ammonia 10 to 10000 times more quickly. The subsurface reservoir from which this cryomagma emerged may have been separate from Pluto's subsurface ocean.{{cite journal |last1=Cruikshank |first1=Dale P. |last2=Umurhan |first2=Orkan M. |last3=Beyer |first3=Ross A. |last4=Schmitt |first4=Bernard |last5=Keane |first5=James T. |last6=Runyon |first6=Kirby D. |last7=Atri |first7=Dimitra |last8=White |first8=Oliver L. |last9=Matsuyama |first9=Isamu |last10=Moore |first10=Jeffrey M. |last11=McKinnon |first11=William B. |last12=Sandford |first12=Scott A. |last13=Singer |first13=Kelsi N. |last14=Grundy |first14=William M. |last15=Dalle Ore |first15=Cristina M.|author15-link=Cristina Dalle Ore |last16=Cook |first16=Jason C. |last17=Bertrand |first17=Tanguy |last18=Stern |first18=S. Alan |last19=Olkin |first19=Catherine B. |last20=Weaver |first20=Harold A. |last21=Young |first21=Leslie A. |last22=Spencer |first22=John R. |last23=Lisse |first23=Carey M. |last24=Binzel |first24=Richard P. |last25=Earle |first25=Alissa M. |last26=Robbins |first26=Stuart J. |last27=Gladstone |first27=G. Randall |last28=Cartwright |first28=Richard J. |last29=Ennico |first29=Kimberly |title=Recent cryovolcanism in Virgil Fossae on Pluto |journal=Icarus |date=15 September 2019 |volume=330 |pages=155–168 |doi=10.1016/j.icarus.2019.04.023 |bibcode=2019Icar..330..155C |s2cid=149983734 |url=https://resolver.caltech.edu/CaltechAUTHORS:20190426-080038903 }}

{{multiple image |caption_align=center |align= center |width= |direction= horizontal

|header= Pluto - possible cryovolcanoes

|image1= PIA20361-Pluto-WrightMons-20150714.jpg

|caption1= Wright Mons (overall context)

|width1= 340

|image2= Pluto possible cryovolcano - Wright Mons.jpg

|caption2= Wright Mons, displaying its central depression ( source image (context))

|width2= 185

|image3= PIA20050-Pluto-IceVolcanoes-20151110.jpg

|caption3= 3D map showing Wright Mons (above) and Piccard Mons

|width3= 100

}}

File:Pluto's internal structure2.jpg

Pluto's density is {{val|1.87|u=g/cm3}}.[http://www.universetoday.com/13861/pluto/ Pluto – Universe Today] Because the decay of radioactive elements would eventually heat the ices enough for the rock to separate from them, scientists think that Pluto's internal structure is differentiated, with the rocky material having settled into a dense core surrounded by a mantle of water ice. Pluto's abundant surface volatiles imply that Pluto is either completely differentiated (and thus has liberated all of the volatiles that had been locked away in its water ice) or formed within less than a million years after the circumstellar disk was cleared (when volatiles were still available to be incorporated into Pluto).{{Cite journal |bibcode = 2020AAS...23543804L|title = Ices in KBO MU69 and Pluto – Implications for Their Formation & Evolution|journal = American Astronomical Society Meeting Abstracts|volume = 52|pages = 438.04|last1 = Lisse|first1 = C. M.|last2 = Young|first2 = L.|last3 = Cruikshank|first3 = D.|last4 = Sandford|first4 = S.|last5 = Schmitt|first5 = B.|last6 = Stern|first6 = S. A.|last7 = Weaver|first7 = H. A.|last8 = Umurhan|first8 = O.|last9 = Pendleton|first9 = Y.|last10 = Keane|first10 = J.|last11 = Gladstone|first11 = R.|last12 = Parker|first12 = J.|last13 = Binzel|first13 = R.|last14 = Earle|first14 = A.|last15 = Horanyi|first15 = M.|last16 = El-Maarry|first16 = M.|last17 = Cheng|first17 = A.|last18 = Moore|first18 = J.|last19 = McKinnon|first19 = W.|last20 = Grundy|first20 = W.|last21 = Kavelaars|first21 = J.|year = 2020}}

The diameter of the core is hypothesized to be approximately {{val|1700|u=km}}, 70% of Pluto's diameter. It is possible that such heating continues today, creating a subsurface ocean layer of liquid water and ammonia some {{nowrap|100 to 180 km}} thick at the core–mantle boundary. Studies based on New Horizon's images of Pluto reveal no signs of contraction (as would be expected if Pluto's internal water had all frozen and turned into ice II) and imply that Pluto's interior is still expanding, probably due to this internal ocean; this is the first concrete evidence that Pluto's interior is still liquid.{{cite news|url=https://www.newscientist.com/article/2094848-pluto-must-have-liquid-ocean-or-itd-look-like-an-overripe-peach/|title=Pluto must have liquid ocean or it'd look like an overripe peach|last=Gearin|first=Conor|work=New Scientist|date=22 June 2016|access-date=23 February 2017}}{{cite journal|last1=Hammond|first1=Noah P.|last2=Barr|first2=Amy C.|last3=Parmentier|first3=Edgar M.|title=Recent tectonic activity on Pluto driven by phase changes in the ice shell|journal=Geophysical Research Letters|date=2 July 2016|volume=43|issue=13|pages=6775–6782|doi=10.1002/2016GL069220|arxiv = 1606.04840 |bibcode = 2016GeoRL..43.6775H |s2cid=54219400}} Pluto is proposed to have a thick water-ice lithosphere, based on the length of individual faults and lack of localized uplift. Differing trends in the faults suggest previously active tectonics, though its mechanisms remain unknown.{{cite journal|last1=Moore|first1=J. M.|last2=McKinnon|first2=W. B.|last3=Spencer|first3=J. R.|last4=Howard|first4=A. D.|last5=Schenk|first5=P. M.|last6=Beyer|first6=R. A.|last7=Nimmo|first7=F.|last8=Singer|first8=K. N.|last9=Umurhan|first9=O. M.|last10=White|first10=O. L.|last11=Stern|first11=S. A.|last12=Ennico|first12=K.|last13=Olkin|first13=C. B.|last14=Weaver|first14=H. A.|last15=Young|first15=L. A.|last16=Binzel|first16=R. P.|last17=Buie|first17=M. W.|last18=Buratti|first18=B. J.|last19=Cheng|first19=A. F.|last20=Cruikshank|first20=D. P.|last21=Grundy|first21=W. M.|last22=Linscott|first22=I. R.|last23=Reitsema|first23=H. J.|last24=Reuter|first24=D. C.|last25=Showalter|first25=M. R.|last26=Bray|first26=V. J.|last27=Chavez|first27=C. L.|last28=Howett|first28=C. J. A.|last29=Lauer|first29=T. R.|last30=Lisse|first30=C. M.|last31=Parker|first31=A. H.|last32=Porter|first32=S. B.|last33=Robbins|first33=S. J.|last34=Runyon|first34=K.|last35=Stryk|first35=T.|last36=Throop|first36=H. B.|last37=Tsang|first37=C. C. C.|last38=Verbiscer|first38=A. J.|last39=Zangari|first39=A. M.|last40=Chaikin|first40=A. L.|last41=Wilhelms|first41=D. E.|display-authors=10|title=The geology of Pluto and Charon through the eyes of New Horizons|journal=Science|date=18 March 2016|volume=351|issue=6279|pages=1284–1293|doi=10.1126/science.aad7055|pmid=26989245|arxiv = 1604.05702 |bibcode = 2016Sci...351.1284M |s2cid=206644622}} The DLR Institute of Planetary Research calculated that Pluto's density-to-radius ratio lies in a transition zone, along with Neptune's moon Triton, between icy satellites like the mid-sized moons of Uranus and Saturn, and rocky satellites such as Jupiter's Io.

Pluto has no magnetic field.{{cite web |title=X-ray Detection Sheds New Light on Pluto |url=https://www.nasa.gov/mission_pages/chandra/x-ray-detection-sheds-new-light-on-pluto.html |access-date=3 December 2016 |date=14 September 2016 |author=NASA |work=nasa.gov}}

{{clear}}

• List of geological features on Pluto

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{{cite web

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{{cite web

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{{cite web

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| access-date = 11 July 2015

}}

[http://solarsystem.dlr.de/TP/aufbau_en.shtml DLR Interior Structure of Planetary Bodies] {{Webarchive|url=https://web.archive.org/web/20110726012828/http://solarsystem.dlr.de/TP/aufbau_en.shtml |date=26 July 2011 }} [http://solarsystem.dlr.de/TP/images/gross/radius_density.jpg DLR Radius to Density] {{Webarchive|url=https://web.archive.org/web/20110726012909/http://solarsystem.dlr.de/TP/images/gross/radius_density.jpg |date=26 July 2011 }} [http://www.dlr.de/pf/en/desktopdefault.aspx/tabid-4772/7910_read-14650/ The natural satellites of the giant outer planets...] {{Webarchive|url=https://web.archive.org/web/20110511145526/http://www.dlr.de/pf/en/desktopdefault.aspx/tabid-4772/7910_read-14650/ |date=11 May 2011 }}

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• [http://www.nasa.gov/image-feature/goddard/views-of-pluto-through-the-years Pluto viewed through the years (NASA; GIF animation; 15 July 2015).]

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Pluto

Category:Geography of Pluto

Category:Pluto