Aeolian bedforms, yardangs, and indurated surfaces in the Tharsis Montes as seen by the HiRISE Camera: Evidence for dust aggregates

N. T. Bridges, M. E. Banks, R. A. Beyer, F. C. Chuang, E. Z. Noe Dobrea, K. E. Herkenhoff, L. P. Keszthelyi, K. E. Fishbaugh, Alfred S. McEwen, T. I. Michaels, B. J. Thomson, J. J. Wray

Research output: Contribution to journalArticle

39 Citations (Scopus)

Abstract

HiRISE images of Mars with ground sampling down to 25 cm/pixel show that the dust-rich mantle covering the surfaces of the Tharsis Montes is organized into ridges whose form and distribution are consistent with formation by aeolian saltation. Other dusty areas near the volcanoes and elsewhere on the planet exhibit a similar morphology. The material composing these "reticulate" bedforms is constrained by their remote sensing properties and the threshold curve combined with the saltation/suspension boundary, both of which vary as a function of elevation (atmospheric pressure), particle size, and particle composition. Considering all of these factors, dust aggregates are the most likely material composing these bedforms. We propose that airfall dust on and near the volcanoes aggregates in situ over time, maybe due to electrostatic charging followed by cementation by salts. The aggregates eventually reach a particle size at which saltation is possible. Aggregates on the flanks are transported downslope by katabatic winds and form linear and "accordion" morphologies. Materials within the calderas and other depressions remain trapped and are subjected to multidirectional winds, forming an interlinked "honeycomb" texture. In many places on and near the volcanoes, light-toned, low thermal inertia yardangs and indurated surfaces are present. These may represent "duststone" formed when aggregates reach a particle size below the threshold curve, such that they become stabilized and subsequently undergo cementation.

Original languageEnglish (US)
Pages (from-to)165-182
Number of pages18
JournalIcarus
Volume205
Issue number1
DOIs
StatePublished - Jan 2010

Fingerprint

bedform
dust
saltation
cameras
volcanoes
cementation
volcano
particle size
thresholds
calderas
curves
caldera
inertia
mars
atmospheric pressure
charging
Mars
remote sensing
ridges
planets

Keywords

  • Mars
  • Surface

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Bridges, N. T., Banks, M. E., Beyer, R. A., Chuang, F. C., Noe Dobrea, E. Z., Herkenhoff, K. E., ... Wray, J. J. (2010). Aeolian bedforms, yardangs, and indurated surfaces in the Tharsis Montes as seen by the HiRISE Camera: Evidence for dust aggregates. Icarus, 205(1), 165-182. https://doi.org/10.1016/j.icarus.2009.05.017

Aeolian bedforms, yardangs, and indurated surfaces in the Tharsis Montes as seen by the HiRISE Camera : Evidence for dust aggregates. / Bridges, N. T.; Banks, M. E.; Beyer, R. A.; Chuang, F. C.; Noe Dobrea, E. Z.; Herkenhoff, K. E.; Keszthelyi, L. P.; Fishbaugh, K. E.; McEwen, Alfred S.; Michaels, T. I.; Thomson, B. J.; Wray, J. J.

In: Icarus, Vol. 205, No. 1, 01.2010, p. 165-182.

Research output: Contribution to journalArticle

Bridges, NT, Banks, ME, Beyer, RA, Chuang, FC, Noe Dobrea, EZ, Herkenhoff, KE, Keszthelyi, LP, Fishbaugh, KE, McEwen, AS, Michaels, TI, Thomson, BJ & Wray, JJ 2010, 'Aeolian bedforms, yardangs, and indurated surfaces in the Tharsis Montes as seen by the HiRISE Camera: Evidence for dust aggregates', Icarus, vol. 205, no. 1, pp. 165-182. https://doi.org/10.1016/j.icarus.2009.05.017
Bridges, N. T. ; Banks, M. E. ; Beyer, R. A. ; Chuang, F. C. ; Noe Dobrea, E. Z. ; Herkenhoff, K. E. ; Keszthelyi, L. P. ; Fishbaugh, K. E. ; McEwen, Alfred S. ; Michaels, T. I. ; Thomson, B. J. ; Wray, J. J. / Aeolian bedforms, yardangs, and indurated surfaces in the Tharsis Montes as seen by the HiRISE Camera : Evidence for dust aggregates. In: Icarus. 2010 ; Vol. 205, No. 1. pp. 165-182.
@article{1570f71c068f4bb3b9e2b12c3af8b188,
title = "Aeolian bedforms, yardangs, and indurated surfaces in the Tharsis Montes as seen by the HiRISE Camera: Evidence for dust aggregates",
abstract = "HiRISE images of Mars with ground sampling down to 25 cm/pixel show that the dust-rich mantle covering the surfaces of the Tharsis Montes is organized into ridges whose form and distribution are consistent with formation by aeolian saltation. Other dusty areas near the volcanoes and elsewhere on the planet exhibit a similar morphology. The material composing these {"}reticulate{"} bedforms is constrained by their remote sensing properties and the threshold curve combined with the saltation/suspension boundary, both of which vary as a function of elevation (atmospheric pressure), particle size, and particle composition. Considering all of these factors, dust aggregates are the most likely material composing these bedforms. We propose that airfall dust on and near the volcanoes aggregates in situ over time, maybe due to electrostatic charging followed by cementation by salts. The aggregates eventually reach a particle size at which saltation is possible. Aggregates on the flanks are transported downslope by katabatic winds and form linear and {"}accordion{"} morphologies. Materials within the calderas and other depressions remain trapped and are subjected to multidirectional winds, forming an interlinked {"}honeycomb{"} texture. In many places on and near the volcanoes, light-toned, low thermal inertia yardangs and indurated surfaces are present. These may represent {"}duststone{"} formed when aggregates reach a particle size below the threshold curve, such that they become stabilized and subsequently undergo cementation.",
keywords = "Mars, Surface",
author = "Bridges, {N. T.} and Banks, {M. E.} and Beyer, {R. A.} and Chuang, {F. C.} and {Noe Dobrea}, {E. Z.} and Herkenhoff, {K. E.} and Keszthelyi, {L. P.} and Fishbaugh, {K. E.} and McEwen, {Alfred S.} and Michaels, {T. I.} and Thomson, {B. J.} and Wray, {J. J.}",
year = "2010",
month = "1",
doi = "10.1016/j.icarus.2009.05.017",
language = "English (US)",
volume = "205",
pages = "165--182",
journal = "Icarus",
issn = "0019-1035",
publisher = "Academic Press Inc.",
number = "1",

}

TY - JOUR

T1 - Aeolian bedforms, yardangs, and indurated surfaces in the Tharsis Montes as seen by the HiRISE Camera

T2 - Evidence for dust aggregates

AU - Bridges, N. T.

AU - Banks, M. E.

AU - Beyer, R. A.

AU - Chuang, F. C.

AU - Noe Dobrea, E. Z.

AU - Herkenhoff, K. E.

AU - Keszthelyi, L. P.

AU - Fishbaugh, K. E.

AU - McEwen, Alfred S.

AU - Michaels, T. I.

AU - Thomson, B. J.

AU - Wray, J. J.

PY - 2010/1

Y1 - 2010/1

N2 - HiRISE images of Mars with ground sampling down to 25 cm/pixel show that the dust-rich mantle covering the surfaces of the Tharsis Montes is organized into ridges whose form and distribution are consistent with formation by aeolian saltation. Other dusty areas near the volcanoes and elsewhere on the planet exhibit a similar morphology. The material composing these "reticulate" bedforms is constrained by their remote sensing properties and the threshold curve combined with the saltation/suspension boundary, both of which vary as a function of elevation (atmospheric pressure), particle size, and particle composition. Considering all of these factors, dust aggregates are the most likely material composing these bedforms. We propose that airfall dust on and near the volcanoes aggregates in situ over time, maybe due to electrostatic charging followed by cementation by salts. The aggregates eventually reach a particle size at which saltation is possible. Aggregates on the flanks are transported downslope by katabatic winds and form linear and "accordion" morphologies. Materials within the calderas and other depressions remain trapped and are subjected to multidirectional winds, forming an interlinked "honeycomb" texture. In many places on and near the volcanoes, light-toned, low thermal inertia yardangs and indurated surfaces are present. These may represent "duststone" formed when aggregates reach a particle size below the threshold curve, such that they become stabilized and subsequently undergo cementation.

AB - HiRISE images of Mars with ground sampling down to 25 cm/pixel show that the dust-rich mantle covering the surfaces of the Tharsis Montes is organized into ridges whose form and distribution are consistent with formation by aeolian saltation. Other dusty areas near the volcanoes and elsewhere on the planet exhibit a similar morphology. The material composing these "reticulate" bedforms is constrained by their remote sensing properties and the threshold curve combined with the saltation/suspension boundary, both of which vary as a function of elevation (atmospheric pressure), particle size, and particle composition. Considering all of these factors, dust aggregates are the most likely material composing these bedforms. We propose that airfall dust on and near the volcanoes aggregates in situ over time, maybe due to electrostatic charging followed by cementation by salts. The aggregates eventually reach a particle size at which saltation is possible. Aggregates on the flanks are transported downslope by katabatic winds and form linear and "accordion" morphologies. Materials within the calderas and other depressions remain trapped and are subjected to multidirectional winds, forming an interlinked "honeycomb" texture. In many places on and near the volcanoes, light-toned, low thermal inertia yardangs and indurated surfaces are present. These may represent "duststone" formed when aggregates reach a particle size below the threshold curve, such that they become stabilized and subsequently undergo cementation.

KW - Mars

KW - Surface

UR - http://www.scopus.com/inward/record.url?scp=72549093656&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=72549093656&partnerID=8YFLogxK

U2 - 10.1016/j.icarus.2009.05.017

DO - 10.1016/j.icarus.2009.05.017

M3 - Article

AN - SCOPUS:72549093656

VL - 205

SP - 165

EP - 182

JO - Icarus

JF - Icarus

SN - 0019-1035

IS - 1

ER -