Seasonal flows on warm Martian slopes

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Reprojected view of warm-season flows in Newton Crater Oblique View of Warm Season Flows in Newton Crater.jpg
Reprojected view of warm-season flows in Newton Crater

Seasonal flows on warm Martian slopes (also called recurring slope lineae, recurrent slope lineae and RSL) [1] [2] are thought to be salty water flows occurring during the warmest months on Mars, or alternatively, dry grains that "flow" downslope of at least 27 degrees.

Contents

The flows are narrow (0.5 to 5 meters) and exhibit relatively dark markings on steep (25° to 40°) slopes, appear and incrementally grow during warm seasons and fade in cold seasons. Liquid brines near the surface have been proposed to explain this activity, [3] or interactions between sulfates and chlorine salts that interact under to produce landslides. [4]

Overview

Research indicates that in the past there was liquid water flowing on the surface of Mars, [5] [6] [7] creating large areas similar to Earth's oceans. [8] [9] [10] [11] However, the question remains as to where the water has gone. [12]

The Mars Reconnaissance Orbiter (MRO) is a multipurpose spacecraft launched in 2005 designed to conduct reconnaissance and exploration of Mars from orbit. [13] The spacecraft is managed by the Jet Propulsion Laboratory (JPL). [14] The HiRISE camera onboard the MRO is at the forefront of the ongoing RSL studies as it helps chart the features with images of closely monitored sites typically taken every few weeks. [15] The 2001 Mars Odyssey orbiter has been using spectrometers and a thermal imager for over 16 years to detect evidence of past or present water and ice. [16] [17] It has detected none at the RSL. [16] On October 5, 2015, possible RSL were reported on Mount Sharp near the Curiosity rover. [2]

Features

Warm season flows on slope in Newton Crater (video-gif) Warm Season Flows on Slope in Newton Crater (animated).gif
Warm season flows on slope in Newton Crater (video-gif)

Distinctive properties of recurring slope lineae (RSL) include slow incremental growth, formation on warm slopes in warm seasons, and annual fading and recurrence, [18] showing a strong correlation with solar heating. [18] RSL extend down slope from bedrock outcrops often following small gullies about 0.5 to 5 meters (1 ft 8 in to 16 ft 5 in) wide, with lengths up to hundreds of meters, and some of the locations display more than 1,000 individual flows. [19] [20] RSL advance rates are highest at the beginning of each season, followed by much slower lengthening. [21] RSL appear and lengthen in the late southern spring and summer from 48°S to 32°S latitudes that favor equator-facing slopes, which are times and places with peak surface temperatures from −23 °C to 27 °C. Active RSL also occur in equatorial regions (0–15°S), most commonly in the Valles Marineris troughs. [21] [22]

Researchers surveyed flow-marked slopes with the Mars Reconnaissance Orbiter 's CRISM and although there is no spectrographic evidence for actual water, [19] the instrument has directly imaged perchlorate salts thought to be dissolved in water brines in the subsurface. [3] This may indicate the water quickly evaporates upon reaching the surface, leaving only the salts. The cause of the surface darkening and lightening is poorly understood: a flow initiated by salty water (brine) could rearrange grains or change surface roughness in a way that darkens the appearance, but the way the features brighten again when temperatures drop is harder to explain. [14] [23] However, in November 2018, it was announced that CRISM had fabricated some additional pixels representing the minerals alunite, kieserite, serpentine and perchlorate. [24] [25] The instrument team found that some false positives were caused by a filtering step when the detector switches from a high luminosity area to shadows. [24] Reportedly, 0.05% of the pixels were indicating perchlorate, now known to be a false high estimate by this instrument. [24] Reduced content of salts on the slopes reduces the chances of the presence of brines. [25]

Hypotheses

A number of different hypotheses for RSL formation have been proposed. The seasonality, latitude distribution, and brightness changes strongly indicate a volatile material—such as water or liquid CO
2—is involved. One hypothesis is that RSL could form by rapid heating of nocturnal frost [18] in agreement with experimental results. [26] Another one proposes flows of carbon dioxide, but the settings in which the flows occur are too warm for carbon-dioxide frost (CO
2), and at some sites is too cold for pure water. [18] Other hypotheses include dry granular flows, but no entirely dry process can explain seasonal flows that progressively grow over weeks and months. [21] Cornice avalanches is another hypothesis. The idea is that wind collects snow or frost just past the peak of a mountain and then this becomes an avalanche after it warms up. Seasonal melting of shallow ice would explain the RSL observations, but it would be difficult to replenish such ice annually. [21] However, as of 2015, direct observations of seasonal deposition of soluble salts strongly suggest that RSL involve brine (hydrated salts). [3]

Brines

The leading hypothesis involves the flow of brines (very salty water). [3] [19] [20] [27] [28] [29] Salt deposits over much of Mars indicate that brine was abundant in Mars's past. [14] [23] Salinity lowers the freezing point of water to sustain a liquid flow. Less saline water would freeze at the observed temperatures. [14] Thermal infrared data from the Thermal Emission Imaging System (THEMIS) on board the 2001 Mars Odyssey orbiter, have allowed the temperature conditions under which RSL form to be constrained. While a small number of RSL are visible at temperatures above the freezing point of water, most are not, and many appear at temperatures as low as −43 °C (230 K). Some scientists think that under these cold conditions, a brine of iron(III) sulfate (Fe2(SO4)3) or calcium chloride (CaCl
2) is the most likely mode of RSL formation. [30] Another team of scientists, using the CRISM instrument onboard MRO, reported that the evidence for hydrated salts is most consistent with the spectral absorption features of magnesium perchlorate (Mg(ClO4)2), magnesium chloride (MgCl2(H2O)x) and sodium perchlorate (NaClO
4). [3] [29]

Experiments and calculations demonstrated that recurring slope lineae could be produced by the deliquescence and rehydration of hydrous chlorides and oxychlorine salts. However, under present Martian atmospheric conditions there is not enough water to complete this process. [31]

These observations are the closest scientists have come to finding evidence of liquid water on the planet's surface today. [14] [23] Frozen water, however, has been detected near the surface in many middle to high-latitude regions. Purported droplets of brine also appeared on struts of the Phoenix Mars Lander in 2008. [32]

Source of water

Liquid brine flows near the surface might explain this activity, but the exact source of the water and the mechanism behind its motion are not understood. [33] [34] A hypothesis proposes that the needed water could originate in the seasonal oscillations of near-surface adsorbed water provided by the atmosphere; perchlorates and other salts known to be present on the surface are able to attract and hold water molecules from the surrounding environment (hygroscopic salts), [21] but the dryness of the Martian air is a challenge. Water vapor must be efficiently trapped over very small areas, and seasonal variation in the atmospheric column abundance of water vapor does not match the RSL activity over active locations. [18] [21]

Deeper groundwater may exist and could reach the surface at springs or seeps, [35] [36] but this cannot explain the wide distribution of RSL, extending from the tops of ridges and peaks. [21] Also, there are apparent RSL on equatorial dunes composed of permeable sand, unlikely to be a groundwater source. [21]

An analysis of near-subsurface data from the Mars Odyssey neutron spectrometer revealed that the RSL sites do not contain any more water than found at anywhere else at similar latitudes. The authors concluded that RSL are not supplied by large, near-surface briny aquifers. It is still possible with this data that water vapor is from deeply buried ice, from the atmosphere, or from small deeply buried aquifers. [16]

Dry sand flows

Dry granular flow was proposed since the first observations of RSLs but this interpretation was ruled out because of the seasonality of the process. The first proposition of a seasonal triggering in a dry context was published in March 2017 using a Knudsen pump effect. [37] The authors demonstrated that the RSLs stopped at an angle of 28° in Garni crater, in agreement with dry granular avalanche. In addition, the authors pointed out several limitations of the wet hypothesis, such as the fact that the detection of water was only indirect (salt detection but not water). This theory pushed back the dry flow theory. Research published in November 2017 concludes that the observations are best explained by dry flow processes, [38] [39] [40] and remark that there is no actual spectrographic evidence for water. [39] [19] Their research shows RSL exist only on slopes steeper than 27 degrees, enough for dry grains to descend the way they do on faces of active dunes. [38] The RSL do not flow onto shallower than 27 degree slopes, which is inconsistent with models for water. [39] A 2016 report also cast doubt on possible sources of underground water at RSL sites, [41] but the new research article acknowledged that hydrated salts could draw some humidity from the atmosphere and seasonal changes in hydration of salt-containing grains might result in some trigger mechanism for RSL grainflows, such as expansion, contraction, or release of some water, that would change the cohesion of grains and cause them to fall or "flow" downslope. [38] Furthermore, neutron spectrometer data by the Mars Odyssey orbiter obtained over one decade, was published in December 2017, and shows no evidence of water (hydrogenated regolith) at the active sites, so its authors also support the hypotheses of either short-lived atmospheric water vapour deliquescence, or dry granular flows. Nevertheless, the footprint of this instrument (~100 km) is much larger than the RSLs (~100m). [16]

Habitability and planetary protection

These features form on Sun-facing slopes at times of the year when the local temperatures reach above the melting point for ice. The streaks grow in spring, widen in late summer and then fade away in autumn. Since these features could involve water in some form, and even though this water could still be too cold or too salty for life, the corresponding areas are currently treated as potentially habitable. Hence they are categorized in planetary protection recommendations as "Uncertain Regions, to be treated as Special Regions" (i.e. a region on the Mars surface where Earth life could potentially survive). [42]

While the wet flows hypothesis has lost some ground since 2015, [24] [25] [38] [39] these regions are still amongst the most favoured candidate sites to support Earth bacteria brought by contaminated landers. Some recurring slope lineae are in reach of the Curiosity rover but planetary protection rules have prevented close exploration by the rover. [2] [43] This has led to some debate about whether these rules should be loosened. [44] [45]

Recurrent slope lineae near equator

See also

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References

  1. ↑ Kirby, Runyon; Ojha, Lujendra (August 18, 2014). "Recurring Slope Lineae". Encyclopedia of Planetary Landforms. p. 1. doi:10.1007/978-1-4614-9213-9_352-1. ISBN   978-1-4614-9213-9.
  2. 1 2 3 Chang, Kenneth (5 October 2015). "Mars Is Pretty Clean. Her Job at NASA Is to Keep It That Way". New York Times . Retrieved 6 October 2015.
  3. 1 2 3 4 5 Ojha, Lujendra; Wilhelm, Mary Beth; Murchie, Scott L.; McEwen, Alfred S.; et al. (28 September 2015). "Spectral evidence for hydrated salts in recurring slope lineae on Mars". Nature Geoscience. 8 (11): 829. Bibcode:2015NatGe...8..829O. doi:10.1038/ngeo2546. S2CID   59152931.
  4. ↑ Bishop, J. L.; Yeşilbaş, M.; Hinman, N. W.; Burton, Z. F. M.; Englert, P. A. J.; Toner, J. D.; McEwen, A. S.; Gulick, V. C.; Gibson, E. K.; Koeberl, C. (2021). "Martian subsurface cryosalt expansion and collapse as trigger for landslides". Science Advances. 7 (6): eabe4459. doi:10.1126/sciadv.abe4459. ISSN   2375-2548. PMC   7857681 . PMID   33536216.
  5. ↑ "Flashback: Water on Mars Announced 10 Years Ago". SPACE.com. June 22, 2000. Retrieved December 19, 2010.
  6. ↑ "Flashback: Water on Mars Announced 10 Years Ago". SPACE.com. June 22, 2010. Retrieved May 13, 2018.
  7. ↑ "Science@NASA, The Case of the Missing Mars Water". Archived from the original on March 27, 2009. Retrieved March 7, 2009.
  8. ↑ Morton, Oliver (2002-10-04). Mapping Mars: Science, Imagination, and the Birth of a World . Picador. ISBN   978-0-312-24551-1.
  9. ↑ "PSRD: Ancient Floodwaters and Seas on Mars". Psrd.hawaii.edu. July 16, 2003. Retrieved December 19, 2010.
  10. ↑ "Gamma-Ray Evidence Suggests Ancient Mars Had Oceans | SpaceRef". SpaceRef. November 17, 2008. Retrieved December 19, 2010.
  11. ↑ Carr, M.; Head, J. (2003). "Oceans on Mars: An assessment of the observational evidence and possible fate". Journal of Geophysical Research. 108 (E5): 5042. Bibcode:2003JGRE..108.5042C. doi: 10.1029/2002JE001963 . S2CID   16367611.
  12. ↑ "Water on Mars: Where is it All?". Archived from the original on December 3, 2007. Retrieved March 7, 2009.
  13. ↑ "Nasa Find Potential Signs Of Flowing Water On Mars". Huffpost UK. August 4, 2011. Retrieved August 5, 2011.
  14. 1 2 3 4 5 "NASA Spacecraft Data Suggest Water Flowing on Mars". Jet Propulsion Laboratory, Pasadena, California. Archived from the original on March 4, 2016. Retrieved March 31, 2012.
  15. ↑ David, Leonard (23 September 2015). "Mars' Mysterious Dark Streaks Spur Exploration Debate". Space.com. Retrieved 2015-09-25.
  16. 1 2 3 4 Equatorial locations of water on Mars: Improved resolution maps based on Mars Odyssey Neutron Spectrometer data (PDF). Jack T. Wilson, Vincent R. Eke, Richard J. Massey, Richard C. Elphic, William C. Feldman, Sylvestre Maurice, Luıs F. A. Teodoroe. Icarus, 299, 148-160. January 2018. Quote: "Finally, we find that the sites of recurring slope lineae (RSL) do not correlate with subsurface hydration. This implies that RSL are not fed by large, near-subsurface aquifers, but are instead the result of either small (<120 km diameter) aquifers, deliquescence of perchlorate and chlorate salts or dry, granular flows."
  17. ↑ "Mars Odyssey Goals". NASA JPL.
  18. 1 2 3 4 5 Dundas, C. M.; McEwen, A. S. (March 16–20, 2015). NEW CONSTRAINTS ON THE LOCATIONS, TIMING AND CONDITIONS FOR RECURRING SLOPE (PDF). 46th Lunar and Planetary Science Conference (2015). Lunar and Planetary Institute.
  19. 1 2 3 4 Mann, Adam (February 18, 2014). "Strange Dark Streaks on Mars Get More and More Mysterious". Wired . Retrieved February 18, 2014.
  20. 1 2 Kerr, Richard A. (August 4, 2011). "Is Mars Weeping Salty Tears?". Science . Retrieved July 14, 2023.
  21. 1 2 3 4 5 6 7 8 McEwen, A.; Chojnacki, M.; Dundas, C.; L. Ojha, L. (28 September 2015). Recurring Slope Lineae on Mars: Atmospheric Origin? (PDF). European Planetary Science Congress 2015. France: EPSC Abstracts.
  22. ↑ Stillman, D., et al. 2016. Characteristics of the Numerous and Widespread Recurring Slope Lineae (RSL) in Valles Marineris, Mars. Icarus: 285, 195-210.
  23. 1 2 3 "NASA Spacecraft Data Suggest Water Flowing on Mars". NASA. Archived from the original on March 4, 2016. Retrieved July 5, 2011.
  24. 1 2 3 4 Mcrae, Mike (22 November 2018), "One of NASA's Mars Exploration Tools Has a Glitch That Created The Illusion of Water", ScienceAlert.com, retrieved 22 November 2018
  25. 1 2 3 An orbiter glitch may mean some signs of liquid water on Mars aren't real. Lisa Grossman, Science News, 21 November 2018.
  26. ↑ Massé, M.; Conway, S.; Gargani, J.; Patel, M.R.; Pasquon, K.; Mc Ewen, A.; Carpy, S.; Chevrier, V.; Balme, M.R.; Ojha, L.; Vincendon, M.; Poulet, F.; Costard, F.; Jouannic, G. (2016). "Transport processes induced by metastable boiling water under Martian surface conditions" (PDF). Nature Geoscience. 9 (6): 425–428. doi:10.1038/ngeo2706.
  27. ↑ "NASA Finds Possible Signs of Flowing Water on Mars". voanews.com. Retrieved August 5, 2011.
  28. ↑ Webster, Guy; Brown, Dwayne (December 10, 2013). "NASA Mars Spacecraft Reveals a More Dynamic Red Planet". NASA . Retrieved December 10, 2013.
  29. 1 2 Wall, Mike (28 September 2015). "Salty Water Flows on Mars Today, Boosting Odds for Life". Space.com. Retrieved 2015-09-28.
  30. ↑ Mitchell, J.; Christensen, P. (March 16–20, 2015). RECURRING SLOPE LINEAE AND THE PRESENCE OF CHLORIDES IN THE SOUTHERN HEMISPHERE OF MARS (PDF). 46th Lunar and Planetary Science Conference (2015). Lunar and Planetary Institute.
  31. ↑ Wang, A.; Ling, Z. C.; Yan, Y. C.; McEwen, A. S.; Mellon, M. T.; Smith, M. D.; Jolliff, B. L.; Head, J. (2017-03-24). "Atmosphere - Surface H2O Exchange to Sustain the Recurring Slope Lineae (RSL) on Mars". Lunar and Planetary Science Conference. 48 (1964): 2351. Bibcode:2017LPI....48.2351W.
  32. ↑ Renno, Nilton; Bos, Brent; et al. (14 October 2009). "Possible physical and thermodynamical evidence for liquid water at the Phoenix landing site" (PDF). J. Geophys. Res. Planets. 114 (E1). Bibcode:2009JGRE..114.0E03R. doi:10.1029/2009JE003362. hdl: 2027.42/95444 .
  33. ↑ McEwen, Alfred.S.; Ojha, Lujendra; Dundas, Colin M. (June 17, 2011). "Seasonal Flows on Warm Martian Slopes". Science. 333 (6043): 740–743. Bibcode:2011Sci...333..740M. doi:10.1126/science.1204816. ISSN   0036-8075. PMID   21817049. S2CID   10460581.
  34. ↑ "Seasonal Flows on Warm Martian Slopes". hirise.lpl.arizona.edu. Retrieved August 5, 2011.
  35. ↑ Levy, Joseph (2012). "Hydrological characteristics of recurrent slope lineae on Mars: Evidence for liquid flow through regolith and comparisons with Antarctic terrestrial analogs". Icarus. 219 (1): 1–4. doi:10.1016/j.icarus.2012.02.016.
  36. ↑ Martín-Torres, F. Javier; Zorzano, María-Paz; Valentín-Serrano, Patricia; Harri, Ari-Matti; Genzer, Maria (13 April 2015). "Transient liquid water and water activity at Gale crater on Mars". Nature Geoscience. 8 (5): 357. Bibcode:2015NatGe...8..357M. doi:10.1038/ngeo2412.
  37. ↑ Schmidt, Frédéric; Andrieu, François; Costard, François; Kocifaj, Miroslav; Meresescu, Alina G. (2017). "Formation of recurring slope lineae on Mars by rarefied gas-triggered granular flows". Nature Geoscience. 10 (4): 270–273. arXiv: 1802.05018 . doi:10.1038/ngeo2917. S2CID   55016186.
  38. 1 2 3 4 Recurring Martian Streaks: Flowing Sand, Not Water?. JPL News, NASA. 20 November 2017.
  39. 1 2 3 4 Dundas, Colin M.; McEwen, Alfred S.; Chojnacki, Matthew; Milazzo, Moses P.; Byrne, Shane; McElwaine, Jim N.; Urso, Anna (2017). "Granular flows at recurring slope lineae on Mars indicate a limited role for liquid water". Nature Geoscience. 10 (12): 903–907. doi:10.1038/s41561-017-0012-5. hdl: 10150/627918 . S2CID   24606098.
  40. ↑ A Mars Mystery: How Did Land Form Without Much Water?. Jan Raack. Space.com. 21 November 2017.
  41. ↑ Mars Canyons Study Adds Clues about Possible Water. JPL News, NASA. 7 July 2016.
  42. ↑ Rummel, John D.; Beaty, David W.; Jones, Melissa A.; Bakermans, Corien; Barlow, Nadine G.; Boston, Penelope J.; Chevrier, Vincent F.; Clark, Benton C.; de Vera, Jean-Pierre P.; Gough, Raina V.; Hallsworth, John E.; Head, James W.; Hipkin, Victoria J.; Kieft, Thomas L.; McEwen, Alfred S.; Mellon, Michael T.; Mikucki, Jill A.; Nicholson, Wayne L.; Omelon, Christopher R.; Peterson, Ronald; Roden, Eric E.; Sherwood Lollar, Barbara; Tanaka, Kenneth L.; Viola, Donna; Wray, James J. (2014). "A New Analysis of liquid "Special Regions": Findings of the Second MEPAG Special Regions Science Analysis Group (SR-SAG2)" (PDF). Astrobiology. 14 (11): 887–968. Bibcode:2014AsBio..14..887R. doi:10.1089/ast.2014.1227. ISSN   1531-1074. PMID   25401393.
  43. ↑ Witze, Alexandra (7 September 2016). "Mars contamination fear could divert Curiosity rover". Nature. 537 (7619): 145–146. doi: 10.1038/537145a . PMID   27604926.
  44. ↑ Fairen, Alberto G.; Parro, Victor; Schulze-Makuch, Dirk; Whyte, Lyle (1 October 2017). "Searching for Life on Mars Before It Is Too Late". Astrobiology. 17 (10): 962–970. doi:10.1089/ast.2017.1703. PMC   5655416 . PMID   28885042.
  45. ↑ Schulze-Makuch, Dirk. "It's Time to Loosen Planetary Protection Rules for Mars". Air and Space magazine. Smithsonian. Retrieved 3 January 2019.
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