Newton (Martian crater)

Martian crater Newton
Gullies inside a small crater within Newton Crater
Planet Mars
Coordinates 40°48′S 201°54′E / 40.8°S 201.9°E / -40.8; 201.9Coordinates: 40°48′S 201°54′E / 40.8°S 201.9°E / -40.8; 201.9
Diameter 298 km
Eponym Sir Isaac Newton

Newton is a large crater on Mars, with a diameter close to 300 km.[1] It is located south of the planet's equator in the heavily cratered highlands of Terra Sirenum in the Phaethontis quadrangle. The crater was named in 1973 by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN) in honor of Sir Isaac Newton.

Topo map photo of Newton crater

Description

The impact that formed Newton likely occurred more than 3 billion years ago. The crater contains smaller craters within its basin and is particularly notable for gully formations that are presumed to be indicative of past liquid water flows. Many small channels exist in this area; they are further evidence of liquid water. On the basis of their form, aspects, positions, and location amongst and apparent interaction with features thought to be rich in water ice, many researchers believed that the processes carving the gullies involve liquid water. However, this remains a topic of active research. As soon as gullies were discovered,[2] researchers began to image many gullies over and over, looking for possible changes. By 2006, some changes were found.[3] Later, with further analysis it was determined that the changes could have occurred by dry granular flows rather than being driven by flowing water.[4][5][6] With continued observations many more changes were found in Gasa Crater and others.[7] With more repeated observations, more and more changes have been found; since the changes occur in the winter and spring, experts are tending to believe that gullies were formed from dry ice. Before-and-after images demonstrated the timing of this activity coincided with seasonal carbon-dioxide frost and temperatures that would not have allowed for liquid water. When dry ice frost changes to a gas, it may lubricate dry material to flow especially on steep slopes.[8][9][10] In some years frost, perhaps as thick as 1 meter.

Oblique view of warm season flows in Newton Crater

In 2011 it was announced that images captured by NASA's Mars Reconnaissance Orbiter have suggested the presence of possible flowing water during the warmest months on Mars, as shown in images taken of Newton Crater and Horowitz Crater among others.

Gullies in crater on rim of Newton Crater, as seen by HiRISE, under HiWish program
Gullies near Newton Crater, as seen by HiRISE under the HiWish Program

Imagery history

The crater now called Newton were taken by Mariner 4 in 1964, the northwesternmost portion and some of its surrounding craters were taken being its 12th close up photo of Mars and the southeast portion being its 13th close up photo. The remainder was taken by Mariner 9 in 1971.

Smaller named craters inside Newton

Two smaller named craters are located inside Newton, Palikir is located south of the crater center, more than halfway to the southern rim and the smaller Avire is located west of the crater center west of Newton's central peak and is nearly halfway between that location and the western rim.

The crater name Palikir (41°34′S 158°52′W / 41.57°S 158.86°W / -41.57; -158.86) was officially named by the IAU in September 2011 and named it after a place in the Federated States of Micronesia,[11] and the crater name Avire (40°49′S 159°46′W / 40.82°S 159.76°W / -40.82; -159.76) was officially named by the IAU in April 2008 and named it after a town in Vanuatu.[12] The diameter for Palikir is 15.57 km[11] and for Avire is 6.85 km.[12] The gullies in Palikir Crater have been thought to show signs that they were carved by running water. This is in contrast to another idea that gullies were made by solid carbon dioxide (dry ice).[13] [14]

Channels

There is enormous evidence that water once flowed in river valleys on Mars.[15][16] Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.[17][18][19][20] Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.[21][22] The pictures below show a channels in Newton Crater.

Dunes

Dunes are also dominant in the middle of the large crater.

See also

References

  1. ↑ http://www.google.com/mars/
  2. ↑ Malin, M., Edgett, K. 2000. Evidence for recent groundwater seepage and surface runoff on Mars. Science 288, 2330–2335.
  3. ↑ Malin, M., K. Edgett, L. Posiolova, S. McColley, E. Dobrea. 2006. Present-day impact cratering rate and contemporary gully activity on Mars. Science 314, 1573_1577.
  4. ↑ Kolb, et al. 2010. Investigating gully flow emplacement mechanisms using apex slopes. Icarus 2008, 132-142.
  5. ↑ McEwen, A. et al. 2007. A closer look at water-related geological activity on Mars. Science 317, 1706-1708.
  6. ↑ Pelletier, J., et al. 2008. Recent bright gully deposits on Mars wet or dry flow? Geology 36, 211-214.
  7. ↑ NASA/Jet Propulsion Laboratory. "NASA orbiter finds new gully channel on Mars." ScienceDaily. ScienceDaily, 22 March 2014. www.sciencedaily.com/releases/2014/03/140322094409.htm
  8. ↑ http://www.jpl.nasa.gov/news/news.php?release=2014-226
  9. ↑ http://hirise.lpl.arizona.edu/ESP_032078_1420
  10. ↑ http://www.space.com/26534-mars-gullies-dry-ice.html
  11. 1 2 "Gazetteer of Planetary Nomenclature | Palikir on Mars". usgs.gov. International Astronomical Union. Retrieved 19 August 2017.
  12. 1 2 "Gazetteer of Planetary Nomenclature | Avire on Mars". usgs.gov. International Astronomical Union. Retrieved 19 August 2017.
  13. ↑ Luu, K., et al. 2018. GULLY FORMATION ON THE NORTHWESTERN SLOPE OF PALIKIR CRATER, MARS 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083). 2650.pdf
  14. ↑ Hamid, S., V. Gulick. 2018. GEOMORPHOLOGICAL ANALYSIS OF GULLIES ALONG WESTERN SLOPES OF PALIKIR CRATER. 49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083). 2644.pdf
  15. ↑ Baker, V., et al. 2015. Fluvial geomorphology on Earth-like planetary surfaces: a review. Geomorphology. 245, 149–182.
  16. ↑ Carr, M. 1996. in Water on Mars. Oxford Univ. Press.
  17. ↑ Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
  18. ↑ Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.
  19. ↑ Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.
  20. ↑ Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.
  21. ↑ http://spaceref.com/mars/how-much-water-was-needed-to-carve-valleys-on-mars.html
  22. ↑ Luo, W., et al. 2017. New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate. Nature Communications 8. Article number: 15766 (2017). doi:10.1038/ncomms15766
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