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Sputnik Planitia

Coordinates: 20°N 180°E / 20°N 180°E / 20; 180
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Sputnik Planitia
New Horizons mosaic of the Sputnik Planitia basin
Feature typePlanitia, impact basin[1]
LocationTombaugh Regio, Pluto
Coordinates20°N 180°E / 20°N 180°E / 20; 180[2]
Diameter1492 km
~1300 km basin diameter[3]
Surface area~5 278 000 km2[a]
Dimensions1400 km × 1200 km[3][b]
DiscovererNew Horizons
EponymSputnik 1 satellite

Sputnik Planitia /ˈspʌtnɪk pləˈnɪʃiə, ˈspʊt-/ (formerly Sputnik Planum)[4] is a large, partially glaciated basin on Pluto. About 1,400 by 1,200 km (870 by 750 mi) in size,[3] Sputnik Planitia is partially submerged in large, bright glaciers of nitrogen ice. Named after Earth's first artificial satellite, Sputnik 1, it constitutes the western lobe of the heart-shaped Tombaugh Regio. Sputnik Planitia lies mostly in the northern hemisphere, but extends across the equator. Much of it has a surface of irregular polygons separated by troughs, interpreted as convection cells in the relatively soft nitrogen ice. The polygons average about 33 km (21 mi) across.[5] In some cases troughs are populated by blocky mountains or hills, or contain darker material.[6] There appear to be windstreaks on the surface with evidence of sublimation.[7][8] The dark streaks are a few kilometers long and all aligned in the same direction.[6] The planitia also contains pits apparently formed by sublimation.[6] No craters were detectable by New Horizons, implying a surface less than 10 million years old.[9] Modeling sublimation pit formation yields a surface age estimate of 180000+90000
−40000 years.[10] Near the northwest margin is a field of transverse dunes (perpendicular to the windstreaks), spaced about 0.4 to 1 km apart, that are thought to be composed of 200-300 μm diameter particles of methane ice derived from the nearby Al-Idrisi Montes.[11][12]

Composition

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The ice composing the basin is thought to consist primarily of nitrogen ice, with smaller fractions of carbon monoxide and methane ice, although relative proportions are uncertain.[13] At Pluto's ambient temperature of 38 K (−235.2 °C; −391.3 °F), nitrogen and carbon monoxide ices are denser and much less rigid than water ice, making glacial-like flows possible; nitrogen ice is the most volatile.[5] The nitrogen ice of the basin rests on Pluto's crust mostly composed of much more rigid water ice.[14]

Origin

[edit]

Sputnik Planitia likely originated as an impact basin that subsequently collected volatile ices.[5] The size of the hypothetical impactor has been estimated as 150–300 km.[1] Alternatively, it has been suggested that the accumulation of ices in this location depressed the surface there, leading to the formation of a basin via a positive feedback process without an impact.[15] The accumulation of several kilometers of nitrogen ice in the basin was in part a consequence of its higher surface pressure, which leads to a higher N2 condensation temperature.[16] The positive temperature gradient of Pluto's atmosphere contributes to making a topographic depression a cold trap.[17][18]

The terrain on Pluto antipodal to Sputnik Planitia may have been altered by the focusing there of seismic energy from the formative impact.[19][20] While this suggestion is tentative in view of the poor resolution of the imaging of the antipodal region, the concept is similar to what has been proposed for areas antipodal to the Caloris basin on Mercury and Mare Orientale on the Moon.

A high seasonal thermal inertia of Pluto's surface is an important driver of deposition of nitrogen ice at low latitudes. These latitudes receive less annual insolation than Pluto's polar regions due to its high obliquity (122.5°).[21] The coldest regions on Pluto, on average, are at 30° N. and S. latitude; early in Pluto's history, ice would tend to accumulate at these latitudes in a runaway process due to the positive feedback association of increased albedo, cooling and further ice deposition (similar to the ice segregation that occurred on Iapetus). Simulations suggest that over a period of about a million years, the runaway process would collect much of the ice into a single cap even in the absence of a preexisting basin.[22]

The accumulation of dense nitrogen ice would have contributed to making Sputnik Planitia a positive gravity anomaly, but by itself would not have been sufficient to overcome the topographic depression associated with the basin. However, other effects of an impact event (see below) could have also contributed to such an anomaly. A positive gravity anomaly could have caused polar wander, reorienting the spin axis of Pluto to put the planitia near the Pluto-Charon tidal axis (the minimum-energy configuration).[17][18] Sputnik Planitia is presently close to the anti-Charon point on Pluto, a result that has less than a 5% probability of arising by chance.[18]

If Sputnik Planitia was created by an impact, then explaining the positive gravity anomaly requires the presence of a subsurface liquid water ocean below Pluto's water ice crust; isostatic uplift of the thinned crust and consequent intrusion of denser liquid water below the basin would account for most of the anomaly.[23] Gradual freezing of such an ocean, in combination with polar wander and the loading of Sputnik Planitia with ice, would also explain the extensional tectonic features seen across Pluto.[18][23] Alternatively, if the accumulation of ice in a single cap (without an impact) created a positive gravity anomaly that reoriented Pluto prior to formation of a basin, the tidal bulge raised by Charon might then have maintained Pluto's orientation even if the positive anomaly later disappeared.[22]

The creation of the gravity anomaly is thought to require thinning the ice crust by ~90 km below Sputnik Planitia. However, the crust must be kept cool to maintain such variations in its thickness. Modeling has suggested that this can be explained if underneath Pluto's water ice crust is a layer of methane hydrate. This clathrate has insulating properties; its thermal conductivity is about 5–10 times less than that of water ice (it also has a viscosity roughly an order of magnitude greater than that of water ice). The additional insulation would help to maintain the layer of water below it in a liquid state, as well as keep the ice crust above it cool. A similar mechanism may contribute to the formation of subsurface oceans on other outer Solar System satellites and trans-Neptunian objects.[14]

Convection cells

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Geologic map of Sputnik Planitia and surroundings (context), with convection cell margins outlined in black

The polygonal structure is a sign of convection of the nitrogen/carbon monoxide ice, with ice warmed by heat from the interior welling up in the center of cells, spreading and then sinking at the ridged margins.[24][25] Convection cells have about 100 m of vertical relief, with the highest points being at their centers.[26][27] Modeling of nitrogen ice convection cells suggests a depth of about one tenth their width, or 3–4 km for most of the planitia, and a maximum flow rate of about 7 cm per year.[5] Cell margins can become pinched off and abandoned as cells evolve.[26] Many of the cells are covered by sublimation pits. These pits grow larger by sublimation during transport from the centers to the edges of convection cells. Using their size distribution, scientists have estimated a convection velocity of 13.8+4.8
−3.8 cm per year, implying a surface age of 180000+90000
−40000 years.[10] Other scientists have proposed that sublimation at the surface of the planitia is responsible for its convection by cooling the surface through latent heat consumption, instead of the driving source from the core originally proposed.[28]

Other obvious indications of ice flow visible in images of the planitia include examples of valley-type glaciers flowing down into the basin from adjacent eastern highlands (the right lobe of Tombaugh Regio), presumably in response to deposition of nitrogen ice there,[13] as well as ice from the planitia flowing into and filling adjacent depressions. The planitia has numerous blocky hills (one to several km across) that form aggregations at cell margins up to 20 km across; these may represent floating chunks of detached water ice crust that were carried onto the planitia by glacial flow and were then collected into troughs by the convection.[5] In some cases the hills seem to form chains along the entry paths of glaciers. The hills may also congregate in nonconvecting regions when they get stuck at locations where the nitrogen ice becomes too shallow.[29]

The planitia has numerous pits that are thought to result from fracturing and sublimation of nitrogen ice; these pits also collect in the margins of convection cells.[5] Often the bottoms of the pits are dark, which may represent an accumulation of tholins left behind by the subliming ice, or a dark substrate below the planitia, if the pits penetrate all the way through the ice. In regions of the planitia where convection cells are not apparent, the pits are more numerous.

Bordering montes

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Annotated map of Sputnik Planitia and surrounding features
A topographic image of the Sputnik Planitia basin, showing the rising scarps bordering the glacial plains. The banding is an artefact of the camera.

On its northwest, Sputnik Planitia is bordered by a chaotic set of blocky mountains, the al-Idrisi Montes, which may have formed via the collapse of adjacent water ice highlands onto the planitia.[5]

On its southwest, the planitia is bordered by the Hillary Montes, rising 1.6 km (0.99 mi; 5,200 ft)[30] above the surface, and, further south, the Tenzing Montes, rising 3.4 km (2.1 mi; 11,000 ft)[31] above the surface. These mountains also have a chaotic, blocky character. The mountains were named after Sir Edmund Hillary, New Zealand mountaineer, and Nepalese Sherpa mountaineer Tenzing Norgay, who were the first climbers to reach the summit of the highest peak on Earth, Mount Everest, on 29 May 1953.[32] Some groups of hills in the basin are named after spacecraft; for example, “Coleta de Dados”, in honor of the first Brazilian satellite launched into space.[33]

Immediately to the southwest of the Tenzing Montes (context) is a large, circular mountain with a central depression, Wright Mons. It has been identified as a possible cryovolcano.[34][35]

Naming

[edit]

The informal name Sputnik Planum was first announced by the New Horizons team on a press conference on 24 July 2015. A planum is a flat region of higher elevation (a plateau). When topographical data was analyzed in early 2016,[36]it became clear that Sputnik is actually a basin, and the informal name was changed to Sputnik Planitia later that year.[4][37] The name was still informal because it had not yet been adopted by the International Astronomical Union (IAU). On 7 September 2017, the name was officially approved together with the names of Tombaugh Regio and 12 other nearby surface features.[38]

See also

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Wikimedia Commons has media related to Sputnik Planitia.

References

[edit]
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  2. ^ "Sputnik Planitia". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  3. ^ a b c d McGovern, P. J.; White, O. L.; Schenk, P. M. (December 2021). "Tectonism and Enhanced Cryovolcanic Potential Around a Loaded Sputnik Planitia Basin, Pluto". Journal of Geophysical Research: Planets. 126 (12). Bibcode:2021JGRE..12606964M. doi:10.1029/2021JE006964.
  4. ^ a b Lakdawalla, Emily (26 October 2016). "DPS/EPSC update on New Horizons at the Pluto system and beyond". The Planetary Society. Retrieved 26 October 2016.
  5. ^ a b c d e f g Lakdawalla, Emily (21 December 2015). "Pluto updates from AGU and DPS: Pretty pictures from a confusing world". The Planetary Society. Retrieved 24 January 2016.
  6. ^ a b c Gary, Stuart (17 July 2015). "NASA'S New Horizons discovers frozen plains in the heart of Pluto's 'Heart'". Retrieved 1 May 2016.
  7. ^ "New Horizons". Pluto.jhuapl.edu. Retrieved 18 July 2015.
  8. ^ Staff (17 July 2015). "NASA – Video (01:20) – Animated flyover of Pluto's icy mountain and plains". NASA & YouTube. Retrieved 18 July 2015.
  9. ^ Marchis, F.; Trilling, D. E. (20 January 2016). "The Surface Age of Sputnik Planum, Pluto, Must Be Less than 10 Million Years". PLOS ONE. 11 (1): e0147386. arXiv:1601.02833. Bibcode:2016PLoSO..1147386T. doi:10.1371/journal.pone.0147386. PMC 4720356. PMID 26790001.
  10. ^ a b Buhler, P. B.; Ingersoll, A. P. (23 March 2017). "Sublimation pit distribution indicates convection cell surface velocity of ~10 centimeters per year in Sputnik Planitia, Pluto" (PDF). 48th Lunar and Planetary Science Conference.
  11. ^ Telfer, M.W.; Parteli, E.R.J.; Radebaugh, J.; et al. (1 June 2018). "Dunes on Pluto". Science. 360 (6392): 992–997. Bibcode:2018Sci...360..992T. doi:10.1126/science.aao2975. PMID 29853681.
  12. ^ Hayes, A.G. (1 June 2018). "Dunes across the Solar System". Science. 360 (6392): 960–961. Bibcode:2018Sci...360..960H. doi:10.1126/science.aat7488. PMID 29853671. S2CID 44138724.
  13. ^ a b Umurhan, O. (8 January 2016). "Probing the Mysterious Glacial Flow on Pluto's Frozen 'Heart'". blogs.nasa.gov. NASA. Retrieved 24 January 2016.
  14. ^ a b Kamata, S.; Nimmo, F.; Sekine, Y.; Kuramoto, K.; Noguchi, N.; Kimura, J.; Tani, A. (2019). "Pluto's ocean is capped and insulated by gas hydrates". Nature Geoscience. 12 (6): 407–410. Bibcode:2019NatGe..12..407K. doi:10.1038/s41561-019-0369-8. hdl:2115/76168. S2CID 182346067.
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  16. ^ Bertrand, T.; Forget, F. (19 September 2016). "Observed glacier and volatile distribution on Pluto from atmosphere–topography processes". Nature. 540 (7631): 86–89. Bibcode:2016Natur.540...86B. doi:10.1038/nature19337. PMID 27629517. S2CID 4401893.
  17. ^ a b Keane, J. T.; Matsuyama, I. (2016). "Pluto followed its heart: true polar wander of Pluto due to the formation and evolution of Sputnik Planum" (PDF). 47th Lunar and Planetary Science Conference. Woodlands, Texas. p. 2348.
  18. ^ a b c d Keane, J. T.; Matsuyama, I.; Kamata, S.; Steckloff, J. K. (16 November 2016). "Reorientation and faulting of Pluto due to volatile loading within Sputnik Planitia". Nature. 540 (7631): 90–93. Bibcode:2016Natur.540...90K. doi:10.1038/nature20120. PMID 27851731. S2CID 4468636.
  19. ^ Andrews, R.G. (26 March 2020). "Collision on One Side of Pluto Ripped Up Terrain on the Other, Study Suggests". ScientificAmerican.com. Scientific American. Retrieved 1 April 2020.
  20. ^ Denton, C.A.; Johnson, B.C.; Freed, A.M.; Melosh, H.J. (2020). Seismology On Pluto?! Antipodal Terrains Produced By Sputnik Planitia-Forming Impact (PDF). 51st Lunar and Planetary Science Conference. Retrieved 1 April 2020.
  21. ^ Bertrand, T.; Forget, F. (19 September 2016). "Observed glacier and volatile distribution on Pluto from atmosphere–topography processes". Nature. 540 (7631): 86–89. Bibcode:2016Natur.540...86B. doi:10.1038/nature19337. PMID 27629517. S2CID 4401893.
  22. ^ a b Hamilton, D. P.; Stern, S. A.; Moore, J. M.; Young, L. A. (30 November 2016). "The rapid formation of Sputnik Planitia early in Pluto's history". Nature. 540 (7631): 97–99. Bibcode:2016Natur.540...97H. doi:10.1038/nature20586. PMID 27905411. S2CID 4457744.
  23. ^ a b Nimmo, F.; et al. (16 November 2016). "Reorientation of Sputnik Planitia implies a subsurface ocean on Pluto". Nature. 540 (7631): 94–96. arXiv:1903.05574. Bibcode:2016Natur.540...94N. doi:10.1038/nature20148. PMID 27851735. S2CID 205251830.
  24. ^ McKinnon, W. B.; et al. (1 June 2016). "Convection in a volatile nitrogen-ice-rich layer drives Pluto's geological vigour". Nature. 534 (7605): 82–85. arXiv:1903.05571. Bibcode:2016Natur.534...82M. doi:10.1038/nature18289. PMID 27251279. S2CID 30903520.
  25. ^ Trowbridge, A. J.; Melosh, H. J.; Steckloff, J. K.; Freed, A. M. (1 June 2016). "Vigorous convection as the explanation for Pluto's polygonal terrain". Nature. 534 (7605): 79–81. Bibcode:2016Natur.534...79T. doi:10.1038/nature18016. PMID 27251278. S2CID 6743360.
  26. ^ a b Keeter, B. (11 January 2016). "'X' Marks a Curious Corner on Pluto's Icy Plains". NASA. Archived from the original on 16 April 2016. Retrieved 24 January 2016.
  27. ^ Kornfeld, L. (9 January 2016). "New high-resolution images show ice flow on Pluto's surface". Spaceflight Insider. Archived from the original on 31 January 2016. Retrieved 25 January 2016.
  28. ^ Morison, Adrien; Labrosse, Stéphane; Choblet, Gaël (16 December 2021). "Sublimation-driven convection in Sputnik Planitia on Pluto". Nature. 600 (7889): 419–423. Bibcode:2021Natur.600..419M. doi:10.1038/s41586-021-04095-w. ISSN 0028-0836. PMID 34912087. S2CID 245219872.
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  31. ^ Nemiroff, R.; Bonnell, J., eds. (18 July 2015). "Fly Over Pluto". Astronomy Picture of the Day. NASA. Retrieved 27 July 2015.
  32. ^ Pokhrel, Rajan (19 July 2015). "Nepal's mountaineering fraternity happy over Pluto mountains named after Tenzing Norgay Sherpa - Nepal's First Landmark In The Solar System". The Himalayan Times. Archived from the original on 13 August 2015. Retrieved 19 July 2015.
  33. ^ "Brasil recebe nomenclatura em Plutão". GOASA. Archived from the original on 8 December 2015.
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  36. ^ "New Elevation Map of Pluto's Sunken 'Heart'". NASA. 29 April 2016. Retrieved 7 September 2017.
  37. ^ "Why Half of Pluto's 'Heart' Has a New Name". space.com. 28 October 2016. Retrieved 7 September 2017.
  38. ^ "Pluto Features Given First Official Names". NASA. 7 September 2017.

Notes

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  1. ^ Calculated using the dimensions provided by MgGovern, White, and Schenk,[3] and the formula for the area of an ellipse:
  2. ^ Glaciated terrain does not cover the entirety of the Sputnik Planitia impact basin
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