Astronomy:Transverse aeolian ridges

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Transverse aeolian ridges (TARs) are visually bright features commonly found in topographic depressions on Mars.[1][2][3] These small-scale and relict bedforms were first seen in narrow-angle images from the Mars Orbiter Camera (MOC)[2][3] and were called “ridges” to preserve both dunes and ripples as formative mechanisms.[2][3] While TARs are widespread on Mars, their formation, age, composition, and role in past Martian sediment cycles remain poorly constrained.[1][2][4][5][6][7]

Aeolian bedforms

Aeolian bedforms are typically classified into either ripples or dunes based on their morphologies and formative mechanisms. Dunes are larger (>0.5 m or taller on Earth[8]), typically asymmetrical in cross-profile, and are the product of hydrodynamic instability related to sand flux, the local topography, shear stress exerted by the wind on sand grains,[9] and flow-form interactions induced by the topography of the dune itself.[10][11][12][13] Wind ripples by comparison are small (amplitudes of 0.6 - 15 mm[14][15][16][17]), are more symmetrical in profile, and are created by saltating and reptating sand grains that tend for form a regular pattern of impact and shadow zones.[8][12][16][17]

On Mars, TARs represent some intermediate form with characteristics of both ripples and dunes. TARs are typically symmetrical in profile[18][19] similar to wind ripples. However, TARs are several orders of magnitude larger than wind ripples observed on Mars or Earth.[20][21][22] TARs are much smaller than Martian dunes, do not have slip-faces, and do not have the characteristic dune stoss and leeslopes. Furthermore, while TARs and dunes have approximately basaltic signatures on Mars,[23] TARs have lower thermal inertias than dunes,[24] indicating that TARs on their surfaces are composed of smaller particles than dunes.[25] Some features on Earth have been proposed as proxies for TARs: gravel megaripples in Argentina ,[26][27] megaripples in Iran[28] and Libya,[29] and reversing dunes in Idaho,[30] but an exact analog remains elusive.

Morphologies

TARs also exhibit a range of morphologies, which are interpreted as representing different formative and evolutionary processes.[2] Past efforts have been made to categorize TAR with classification systems primarily focusing on crest morphology.[2][3]

The morphologies of Transverse Aeolian ridges
Morphology Description Example image HiRISE image source
Simple Straight parallel crests
Simple TARs.jpg
https://www.uahirise.org/ESP_045814_1520
Forked Straight parallel crests with forking
Forked TARs.jpg
https://www.uahirise.org/ESP_045814_1520
Sinuous Winding but non-overlapping crests
Sinuous TARs.jpg
https://www.uahirise.org/PSP_002824_1355
Barchan-like Relatively short crests bent at ~90-150º
Barchan TARs.jpg
https://www.uahirise.org/ESP_036410_1810
Networked Highly connected ridge crests that form closed irregular polygonal shapes
Networked TARs.jpg
https://www.uahirise.org/PSP_002824_1355
Feathered[2][31][32]* Large primary ridge with smaller secondary ridges approximately perpendicular to the main crest

*Established in the literature but not recognized as a distinct morphology

Formation

There are competing hypotheses for TAR formation.[2][19][26][28][29][30][33][34] Granule ripples covered by a monolayer of coarse millimeter-sized particles have been proposed for smaller TARs (amplitude <1 m),[22][33][35][36] while dust-covered reversing dunes have been proposed for TARs >1 m in amplitude.[37][30]

Past climate

Understanding TAR formation and evolution could offer insight into the winds that created them.[38] In turn, these inferences could have further insights into past wind patterns, atmospheric compositions, and climatic dynamics generally on Mars.[38] Relict aeolian features exist on Earth and are useful records of local and atmospheric conditions, but the rapid erosion rates on Earth erase aeolian features older than the approximately the Last Glacial Maximum.[39][40][41][42] Resurfacing rates are much slower on Mars so TARs could preserve conditions considerably further back in the Martian past.

Current activity

A 2020 study found evidence that some isolated TARs could still be minimally active (i.e. ridge crests that are moving or changing), but the literature suggests that the majority of TARs are immobile.[43] For example, dunes have been observed passing over TARs with no change to the underlying TARs after the dune's passing.[1][2]

Images of TARs

  • Yardangs, as seen by HiRISE under HiWish program. Location is Arsinoes Chaos. The next image shows part of this enlarged so that TAR's can be seen.

  • Close-up of yardangs, as seen by HiRISE under HiWish program. Arrows point to sand ridges that are called "transverse aeolian ridges" (TAR's).

  • Layers in depression in crater, as seen by HiRISE under HiWish program A special type of sand ripple called Transverse aeolian ridges, TAR's are visible and labeled. Location is Hellas Planitia in Noachis quadrangle.

  • Close, color view of unusual transverse aeolian ridges, TAR's, as seen by HiRISE under HiWish program These features may have had variable local winds to make the wavy tops.

  • Close view of TAR's with waves, as seen by HiRISE under HiWish program

  • Close, color view of TAR's in a channel,as seen by HiRISE under HiWish program Only part of the image is in color because HiRISE only takes a 1 km wide color strip.

See also

References

  1. ↑ 1.0 1.1 1.2 Berman, Daniel C.; Balme, Matthew R.; Rafkin, Scot C.R.; Zimbelman, James R. (2011). "Transverse Aeolian Ridges (TARs) on Mars II: Distributions, orientations, and ages". Icarus 213 (1): 116–130. doi:10.1016/j.icarus.2011.02.014. ISSN 0019-1035. Bibcode: 2011Icar..213..116B. http://dx.doi.org/10.1016/j.icarus.2011.02.014. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 Balme, Matt; Berman, Daniel C.; Bourke, Mary C.; Zimbelman, James R. (2008). "Transverse Aeolian Ridges (TARs) on Mars". Geomorphology 101 (4): 703–720. doi:10.1016/j.geomorph.2008.03.011. ISSN 0169-555X. Bibcode: 2008Geomo.101..703B. http://dx.doi.org/10.1016/j.geomorph.2008.03.011. 
  3. ↑ 3.0 3.1 3.2 3.3 Wilson, Sharon A. (2004). "Latitude-dependent nature and physical characteristics of transverse aeolian ridges on Mars" (in en). Journal of Geophysical Research 109 (E10): E10003. doi:10.1029/2004JE002247. ISSN 0148-0227. Bibcode: 2004JGRE..10910003W. http://doi.wiley.com/10.1029/2004JE002247. 
  4. ↑ Bridges, N. T.; Bourke, M. C.; Geissler, P. E.; Banks, M. E.; Colon, C.; Diniega, S.; Golombek, M. P.; Hansen, C. J. et al. (2012). "Planet-wide sand motion on Mars" (in en). Geology 40 (1): 31–34. doi:10.1130/G32373.1. ISSN 0091-7613. Bibcode: 2012Geo....40...31B. https://pubs.geoscienceworld.org/geology/article/40/1/31-34/130678. 
  5. ↑ Geissler, Paul E.; Wilgus, Justin T. (2017). "The morphology of transverse aeolian ridges on Mars" (in en). Aeolian Research 26: 63–71. doi:10.1016/j.aeolia.2016.08.008. Bibcode: 2017AeoRe..26...63G. https://linkinghub.elsevier.com/retrieve/pii/S1875963716300404. 
  6. ↑ Geissler, Paul E. (2014). "The birth and death of transverse aeolian ridges on Mars: Transverse Aeolian Ridges on Mars" (in en). Journal of Geophysical Research: Planets 119 (12): 2583–2599. doi:10.1002/2014JE004633. 
  7. ↑ Wilson, Sharon A. (2015), Hargitai, Henrik; Kereszturi, Ákos, eds. (in en), Transverse Aeolian Ridge (TAR), New York, NY: Springer, pp. 2177–2185, doi:10.1007/978-1-4614-3134-3_380, ISBN 978-1-4614-3134-3, https://doi.org/10.1007/978-1-4614-3134-3_380, retrieved 2020-09-16 
  8. ↑ 8.0 8.1 Vriend, N. M.; Jarvis, P. A. (2018). "Between a ripple and a dune" (in en). Nature Physics 14 (7): 641–642. doi:10.1038/s41567-018-0113-0. ISSN 1745-2473. Bibcode: 2018NatPh..14..641V. http://www.nature.com/articles/s41567-018-0113-0. 
  9. ↑ WILSON, IAN G. (1972). "Aeolian Bedforms-Their Development and Origins". Sedimentology 19 (3–4): 173–210. doi:10.1111/j.1365-3091.1972.tb00020.x. ISSN 0037-0746. Bibcode: 1972Sedim..19..173W. http://dx.doi.org/10.1111/j.1365-3091.1972.tb00020.x. 
  10. ↑ Cooper, William S. (1958), "Coastal Sand Dunes of Oregon and Washington" (in en), 72 : Coastal Sand Dunes of Oregon and Washington, Geological Society of America Memoirs, 72, Geological Society of America, pp. 1–162, doi:10.1130/mem72-p1, https://pubs.geoscienceworld.org/books/book/79/chapter/3788036/, retrieved 2020-09-15 
  11. ↑ G. Kocurek, M. Townsley, E. Yeh, K. (1992). "Dune and Dune-Field Development on Padre Island, Texas, with Implications for Interdune Deposition and Water-Table-Controlled Accumulation". SEPM Journal of Sedimentary Research 62. doi:10.1306/d4267974-2b26-11d7-8648000102c1865d. ISSN 1527-1404. http://dx.doi.org/10.1306/d4267974-2b26-11d7-8648000102c1865d. 
  12. ↑ 12.0 12.1 Bagnold, R. A. (2012). Physics of Blown Sand and Desert Dunes.. Dover Publications. ISBN 978-1-306-35507-0. OCLC 868966351. https://www.worldcat.org/oclc/868966351. 
  13. ↑ Werner, B. T. (1995). "Eolian dunes: Computer simulations and attractor interpretation" (in en). Geology 23 (12): 1107–1110. doi:10.1130/0091-7613(1995)023<1107:EDCSAA>2.3.CO;2. ISSN 0091-7613. Bibcode: 1995Geo....23.1107W. https://pubs.geoscienceworld.org/gsa/geology/article-abstract/23/12/1107/206230/Eolian-dunes-Computer-simulations-and-attractor. 
  14. ↑ Anderson, R (1990). "Eolian ripples as examples of self-organization in geomorphological systems" (in en). Earth-Science Reviews 29 (1–4): 77–96. doi:10.1016/0012-8252(0)90029-U. https://linkinghub.elsevier.com/retrieve/pii/001282529090029U. 
  15. ↑ Boulton, J. Wayne (1997). Quantifying the morphology of aeolian impact ripples formed in a natural dune setting. National Library of Canada = Bibliothèque nationale du Canada. OCLC 654186636. http://worldcat.org/oclc/654186636. 
  16. ↑ 16.0 16.1 Sharp, Robert P. (1963). "Wind Ripples" (in en). The Journal of Geology 71 (5): 617–636. doi:10.1086/626936. ISSN 0022-1376. Bibcode: 1963JG.....71..617S. https://www.journals.uchicago.edu/doi/10.1086/626936. 
  17. ↑ 17.0 17.1 Wang, Peng; Zhang, Jie; Huang, Ning (2019). "A theoretical model for aeolian polydisperse-sand ripples" (in en). Geomorphology 335: 28–36. doi:10.1016/j.geomorph.2019.03.013. Bibcode: 2019Geomo.335...28W. 
  18. ↑ Zimbelman, J. R.; Williams, S. H. (2007-07-01). "An Evaluation of Formation Processes for Transverse Aeolian Ridges on Mars". Seventh International Conference on Mars 1353: 3047. Bibcode: 2007LPICo1353.3047Z. http://adsabs.harvard.edu/abs/2007LPICo1353.3047Z. 
  19. ↑ 19.0 19.1 Shockey, K. M.; Zimbelman, J. R. (2012-09-20). "Analysis of transverse aeolian ridge profiles derived from HiRISE images of Mars". Earth Surface Processes and Landforms 38 (2): 179–182. doi:10.1002/esp.3316. ISSN 0197-9337. http://dx.doi.org/10.1002/esp.3316. 
  20. ↑ Bourke, M.C.; Balme, M.; Beyer, R.A.; Williams, K.K.; Zimbelman, J. (2006). "A comparison of methods used to estimate the height of sand dunes on Mars". Geomorphology 81 (3–4): 440–452. doi:10.1016/j.geomorph.2006.04.023. ISSN 0169-555X. Bibcode: 2006Geomo..81..440B. http://dx.doi.org/10.1016/j.geomorph.2006.04.023. 
  21. ↑ Claudin, Philippe; Andreotti, Bruno (2006). "A scaling law for aeolian dunes on Mars, Venus, Earth, and for subaqueous ripples". Earth and Planetary Science Letters 252 (1–2): 30–44. doi:10.1016/j.epsl.2006.09.004. ISSN 0012-821X. Bibcode: 2006E&PSL.252...30C. http://dx.doi.org/10.1016/j.epsl.2006.09.004. 
  22. ↑ 22.0 22.1 Williams, S. H.; Zimbelman, J. R.; Ward, A. W. (2002). "Large Ripples on Earth and Mars". Lunar and Planetary Science Conference 33: 1508. Bibcode: 2002LPI....33.1508W. http://adsabs.harvard.edu/abs/2002LPI....33.1508W. 
  23. ↑ Fenton, Lori K.; Bandfield, Joshua L.; Ward, A. Wesley (2003). "Aeolian processes in Proctor Crater on Mars: Sedimentary history as analyzed from multiple data sets". Journal of Geophysical Research: Planets 108 (E12): 5129. doi:10.1029/2002je002015. ISSN 0148-0227. Bibcode: 2003JGRE..108.5129F. http://dx.doi.org/10.1029/2002je002015. 
  24. ↑ Fenton, Lori K.; Mellon, Michael T. (2006). "Thermal properties of sand from Thermal Emission Spectrometer (TES) and Thermal Emission Imaging System (THEMIS): Spatial variations within the Proctor Crater dune field on Mars". Journal of Geophysical Research 111 (E6): E06014. doi:10.1029/2004je002363. ISSN 0148-0227. Bibcode: 2006JGRE..111.6014F. http://dx.doi.org/10.1029/2004je002363. 
  25. ↑ Presley, Marsha A.; Christensen, Philip R. (1997-03-25). "Thermal conductivity measurements of particulate materials 1. A review" (in en). Journal of Geophysical Research: Planets 102 (E3): 6535–6549. doi:10.1029/96JE03302. Bibcode: 1997JGR...102.6535P. 
  26. ↑ 26.0 26.1 de Silva, S. L.; Spagnuolo, M. G.; Bridges, N. T.; Zimbelman, J. R. (2013-10-31). "Gravel-mantled megaripples of the Argentinean Puna: A model for their origin and growth with implications for Mars". Geological Society of America Bulletin 125 (11–12): 1912–1929. doi:10.1130/b30916.1. ISSN 0016-7606. Bibcode: 2013GSAB..125.1912D. http://dx.doi.org/10.1130/b30916.1. 
  27. ↑ Montgomery, David R.; Bandfield, Joshua L.; Becker, Scott K. (2012). "Periodic bedrock ridges on Mars". Journal of Geophysical Research: Planets 117 (E3): n/a. doi:10.1029/2011je003970. ISSN 0148-0227. Bibcode: 2012JGRE..117.3005M. http://dx.doi.org/10.1029/2011je003970. 
  28. ↑ 28.0 28.1 Foroutan, M.; Zimbelman, J.R. (2016). "Mega-ripples in Iran: A new analog for transverse aeolian ridges on Mars". Icarus 274: 99–105. doi:10.1016/j.icarus.2016.03.025. ISSN 0019-1035. Bibcode: 2016Icar..274...99F. http://dx.doi.org/10.1016/j.icarus.2016.03.025. 
  29. ↑ 29.0 29.1 Foroutan, M.; Steinmetz, G.; Zimbelman, J.R.; Duguay, C.R. (2019). "Megaripples at Wau-an-Namus, Libya: A new analog for similar features on Mars". Icarus 319: 840–851. doi:10.1016/j.icarus.2018.10.021. ISSN 0019-1035. Bibcode: 2019Icar..319..840F. http://dx.doi.org/10.1016/j.icarus.2018.10.021. 
  30. ↑ 30.0 30.1 30.2 Zimbelman, James R.; Scheidt, Stephen P. (2014). "Precision topography of a reversing sand dune at Bruneau Dunes, Idaho, as an analog for Transverse Aeolian Ridges on Mars". Icarus 230: 29–37. doi:10.1016/j.icarus.2013.08.004. ISSN 0019-1035. Bibcode: 2014Icar..230...29Z. http://dx.doi.org/10.1016/j.icarus.2013.08.004. 
  31. ↑ Berman, Daniel C.; Balme, Matthew R.; Michalski, Joseph R.; Clark, Stacey C.; Joseph, Emily C.S. (2018). "High-resolution investigations of Transverse Aeolian Ridges on Mars" (in en). Icarus 312: 247–266. doi:10.1016/j.icarus.2018.05.003. Bibcode: 2018Icar..312..247B. https://linkinghub.elsevier.com/retrieve/pii/S0019103517305857. 
  32. ↑ Bhardwaj, Anshuman; Sam, Lydia; Martin-Torres, F. Javier; Zorzano, Maria-Paz (2019). "Distribution and Morphologies of Transverse Aeolian Ridges in ExoMars 2020 Rover Landing Site" (in en). Remote Sensing 11 (8): 912. doi:10.3390/rs11080912. ISSN 2072-4292. Bibcode: 2019RemS...11..912B. 
  33. ↑ 33.0 33.1 Hugenholtz, Chris H.; Barchyn, Thomas E.; Boulding, Adam (2017). "Morphology of transverse aeolian ridges (TARs) on Mars from a large sample: Further evidence of a megaripple origin?". Icarus 286: 193–201. doi:10.1016/j.icarus.2016.10.015. ISSN 0019-1035. Bibcode: 2017Icar..286..193H. http://dx.doi.org/10.1016/j.icarus.2016.10.015. 
  34. ↑ Montgomery, David R.; Bandfield, Joshua L.; Becker, Scott K. (2012). "Periodic bedrock ridges on Mars". Journal of Geophysical Research: Planets 117 (E3): n/a. doi:10.1029/2011je003970. ISSN 0148-0227. Bibcode: 2012JGRE..117.3005M. http://dx.doi.org/10.1029/2011je003970. 
  35. ↑ Lämmel, Marc; Meiwald, Anne; Yizhaq, Hezi; Tsoar, Haim; Katra, Itzhak; Kroy, Klaus (2018-04-30). "Aeolian sand sorting and megaripple formation". Nature Physics 14 (7): 759–765. doi:10.1038/s41567-018-0106-z. ISSN 1745-2473. Bibcode: 2018NatPh..14..759L. http://dx.doi.org/10.1038/s41567-018-0106-z. 
  36. ↑ Wilson, S. A.; Zimbelman, J. R.; Williams, S. H. (2003-03-01). "Large Aeolian Ripples: Extrapolations from Earth to Mars". Lunar and Planetary Science Conference 34: 1862. Bibcode: 2003LPI....34.1862W. http://adsabs.harvard.edu/abs/2003LPI....34.1862W. 
  37. ↑ Zimbelman, James R. (2010). "Transverse Aeolian Ridges on Mars: First results from HiRISE images". Geomorphology 121 (1–2): 22–29. doi:10.1016/j.geomorph.2009.05.012. ISSN 0169-555X. Bibcode: 2010Geomo.121...22Z. http://dx.doi.org/10.1016/j.geomorph.2009.05.012. 
  38. ↑ 38.0 38.1 Gardin, Emilie; Allemand, Pascal; Quantin, Cathy; Silvestro, Simone; Delacourt, Christophe (2012). "Dune fields on Mars: Recorders of a climate change?" (in en). Planetary and Space Science. Titan Through Time: A Workshop on Titan’s Formation, Evolution and Fate 60 (1): 314–321. doi:10.1016/j.pss.2011.10.004. ISSN 0032-0633. Bibcode: 2012P&SS...60..314G. http://www.sciencedirect.com/science/article/pii/S0032063311003059. 
  39. ↑ BEVERIDGE, CARRIE; KOCUREK, GARY; EWING, RYAN C.; LANCASTER, NICHOLAS; MORTHEKAI, P.; SINGHVI, ASHOK K.; MAHAN, SHANNON A. (2006). "Development of spatially diverse and complex dune-field patterns: Gran Desierto Dune Field, Sonora, Mexico". Sedimentology 53 (6): 1391–1409. doi:10.1111/j.1365-3091.2006.00814.x. ISSN 0037-0746. Bibcode: 2006Sedim..53.1391B. http://dx.doi.org/10.1111/j.1365-3091.2006.00814.x. 
  40. ↑ KOCUREK, GARY; HAVHOLM, KAREN G.; DEYNOUX, MAX; BLAKEY, RONALD C. (1991). "Amalgamated accumulations resulting from climatic and eustatic changes, Akchar Erg, Mauritania". Sedimentology 38 (4): 751–772. doi:10.1111/j.1365-3091.1991.tb01018.x. ISSN 0037-0746. Bibcode: 1991Sedim..38..751K. http://dx.doi.org/10.1111/j.1365-3091.1991.tb01018.x. 
  41. ↑ Swezey, Christopher S. (2003). "Late Pleistocene and Holocene dune activity and wind regimes in the western Sahara Desert of Mauritania: Comment and Reply". Geology 31 (1): e18. doi:10.1130/0091-7613-31.1.e18. ISSN 1943-2682. 
  42. ↑ Wolfe, Stephen A.; Huntley, David J.; Ollerhead, Jeff (2006-07-18). "Relict Late Wisconsinan Dune Fields of the Northern Great Plains, Canada*". Géographie Physique et Quaternaire 58 (2–3): 323–336. doi:10.7202/013146ar. ISSN 1492-143X. 
  43. ↑ Silvestro, S.; Chojnacki, M.; Vaz, D. A.; Cardinale, M.; Yizhaq, H.; Esposito, F. (2020). "Megaripple Migration on Mars" (in en). Journal of Geophysical Research: Planets 125 (8): e2020JE006446. doi:10.1029/2020JE006446. ISSN 2169-9097. PMID 33133993. Bibcode: 2020JGRE..12506446S. 



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