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Jackson B. On the Relationship between Dust Devil Radii and Heights. ICARUS 2020; 338:113523. [PMID: 31806915 PMCID: PMC6894178 DOI: 10.1016/j.icarus.2019.113523] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
The influence of dust devils on the martian atmosphere depends on their capacity to loft dust, which depends on their wind profiles and footprint on the martian surface, i.e., on their radii, R. Previous work suggests the wind profile depends on a devil's thermodynamic efficiency, which scales with its height, h. However, the precise mechanisms that set a dust devil's radius have remained unclear. Combining previous work with simple assumptions about angular momentum conservation in dust devils predicts that R ∝ h 1/2, and a model fit to observed radii and heights from a survey of martian dust devils using the Mars Express High Resolution Stereo Camera agrees reasonably well with this prediction. Other observational tests involving additional, statistically robust dust devil surveys and field measurements may further elucidate these relationships.
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Affiliation(s)
- Brian Jackson
- Boise State University, Dept. of Physics 1910 University Drive, Boise ID 83725-1570
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Martínez-Pabello PU, Navarro-González R, Walls X, Pi-Puig T, González-Chávez JL, de la Rosa JG, Molina P, Zamora O. Production of nitrates and perchlorates by laser ablation of sodium chloride in simulated Martian atmospheres. Implications for their formation by electric discharges in dust devils. LIFE SCIENCES IN SPACE RESEARCH 2019; 22:125-136. [PMID: 31421844 DOI: 10.1016/j.lssr.2019.02.007] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/24/2018] [Revised: 02/25/2019] [Accepted: 02/25/2019] [Indexed: 06/10/2023]
Abstract
Nitrates and perchlorates are present both on Earth and Mars. In the Martian environment perchlorates dominate over nitrates whereas on Earth is contrariwise. This implies that the mechanisms responsible for their formation are different for both planets. The chemical elements required for their formation are nitrogen and chlorine, which are present in the atmosphere and surface, respectively. Dust in the Martian atmosphere causes atmospheric perturbations that lead to the development of dust-devils and sandstorms. Dust devils contain both chemical elements simultaneously, and normally generate high electric fields that can trigger the formation of electric discharges. Here we present laboratory experiments of this phenomenon using laser ablation of a sodium chloride (NaCl) plate in two different simulated atmospheres: (1) 96% CO2, 2% N2 and 2% Ar; and (2) 66% CO2, 33% N2 and 1% Ar. The dust that condensed and accumulated on the walls of the reactor was analyzed by different analytical techniques that included Fourier transform infrared spectroscopy, visible spectroscopy using azo dyes, thermogravimetry/simultaneous thermal analyses coupled to mass spectrometry, powder X-ray diffraction, and ion chromatography. The main components of the ablated dust corresponded to NaCl ≥ 91.5%, sodium nitrate (NaNO3 = 1.6-6.0%), and sodium perchlorate (NaClO4 ∼ 0.2-0.3%). It is interesting to note that these salts formed in a dry process that is relevant to Mars today. A thermochemical model was used to understand the chemical steps that led to the formation of these salts in the gas phase. The NaNO3NaClO4 (wt/wt) ratio of this process was estimated to vary from 5.0 to 30.0; this ratio is too high compared to that found on Mars (NO3-ClO4- (wt/wt)) from 0.004 to 0.13). This implies that gaseous NaCl was not efficiently oxidized to perchlorate by the electric discharge process. We propose instead that gaseous metal chlorides (e.g., MgCl2, NaCl, CaCl2, KCl) were supplied to the atmosphere by the volatilization of chloride minerals present in the dust by electric discharges generated in dust devils and were subsequently oxidized to perchlorate by photochemical processes. Further work is required to assess the relative contribution of this possible source.
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Affiliation(s)
- Pável U Martínez-Pabello
- Laboratorio de Química de Plasmas y Estudios Planetarios, Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior, Ciudad Universitaria, Apartado Postal 70-543, Coyoacán, Ciudad de México 04510, Mexico
| | - Rafael Navarro-González
- Laboratorio de Química de Plasmas y Estudios Planetarios, Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior, Ciudad Universitaria, Apartado Postal 70-543, Coyoacán, Ciudad de México 04510, Mexico.
| | - Xavier Walls
- Laboratorio de Química de Plasmas y Estudios Planetarios, Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior, Ciudad Universitaria, Apartado Postal 70-543, Coyoacán, Ciudad de México 04510, Mexico
| | - Teresa Pi-Puig
- Departamento de Geoquímica, Instituto de Geología y LANGEM (Laboratorio Nacional de Geoquímica y Mineralogía), Universidad Nacional Autónoma de México, Ciudad Universitaria 04510, Coyoacán, Ciudad de México 04510, Mexico
| | - José L González-Chávez
- Departamento de Química Analítica, Facultad de Química, Universidad Nacional Autónoma de México, Ciudad Universitaria, Coyoacán, Ciudad de México 04510, Mexico
| | - José G de la Rosa
- Laboratorio de Química de Plasmas y Estudios Planetarios, Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior, Ciudad Universitaria, Apartado Postal 70-543, Coyoacán, Ciudad de México 04510, Mexico
| | - Paola Molina
- Laboratorio de Química de Plasmas y Estudios Planetarios, Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior, Ciudad Universitaria, Apartado Postal 70-543, Coyoacán, Ciudad de México 04510, Mexico
| | - Olivia Zamora
- Departamento de Ciencias Ambientales y del Suelo, Instituto de Geología y LANGEM, Universidad Nacional Autónoma de México, Ciudad Universitaria 04510, Coyoacán, Ciudad de México 04510, Mexico
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Using an Instrumented Drone to Probe Dust Devils on Oregon’s Alvord Desert. REMOTE SENSING 2018. [DOI: 10.3390/rs10010065] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
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Greeley R, Waller DA, Cabrol NA, Landis GA, Lemmon MT, Neakrase LDV, Pendleton Hoffer M, Thompson SD, Whelley PL. Gusev Crater, Mars: Observations of three dust devil seasons. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010je003608] [Citation(s) in RCA: 70] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Ellehoj MD, Gunnlaugsson HP, Taylor PA, Kahanpää H, Bean KM, Cantor BA, Gheynani BT, Drube L, Fisher D, Harri AM, Holstein-Rathlou C, Lemmon MT, Madsen MB, Malin MC, Polkko J, Smith PH, Tamppari LK, Weng W, Whiteway J. Convective vortices and dust devils at the Phoenix Mars mission landing site. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003413] [Citation(s) in RCA: 92] [Impact Index Per Article: 6.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Towner MC. Characteristics of large Martian dust devils using Mars Odyssey Thermal Emission Imaging System visual and infrared images. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003220] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Greeley R, Whelley PL, Arvidson RE, Cabrol NA, Foley DJ, Franklin BJ, Geissler PG, Golombek MP, Kuzmin RO, Landis GA, Lemmon MT, Neakrase LDV, Squyres SW, Thompson SD. Active dust devils in Gusev crater, Mars: Observations from the Mars Exploration Rover Spirit. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002743] [Citation(s) in RCA: 114] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Ronald Greeley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | - Patrick L. Whelley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University in St. Louis; St. Louis Missouri USA
| | | | - Daniel J. Foley
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | | | - Paul G. Geissler
- Astrogeology Program; U.S. Geological Survey; Flagstaff Arizona USA
| | | | | | | | - Mark T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - Lynn D. V. Neakrase
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
| | | | - Shane D. Thompson
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
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Cantor BA, Kanak KM, Edgett KS. Mars Orbiter Camera observations of Martian dust devils and their tracks (September 1997 to January 2006) and evaluation of theoretical vortex models. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002700] [Citation(s) in RCA: 116] [Impact Index Per Article: 6.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | - Katharine M. Kanak
- Cooperative Institute for Mesoscale Meteorological Studies; University of Oklahoma; Norman Oklahoma USA
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Atreya SK, Wong AS, Renno NO, Farrell WM, Delory GT, Sentman DD, Cummer SA, Marshall JR, Rafkin SCR, Catling DC. Oxidant enhancement in martian dust devils and storms: implications for life and habitability. ASTROBIOLOGY 2006; 6:439-50. [PMID: 16805700 DOI: 10.1089/ast.2006.6.439] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/10/2023]
Abstract
We investigate a new mechanism for producing oxidants, especially hydrogen peroxide (H2O2), on Mars. Large-scale electrostatic fields generated by charged sand and dust in the martian dust devils and storms, as well as during normal saltation, can induce chemical changes near and above the surface of Mars. The most dramatic effect is found in the production of H2O2 whose atmospheric abundance in the "vapor" phase can exceed 200 times that produced by photochemistry alone. With large electric fields, H2O2 abundance gets large enough for condensation to occur, followed by precipitation out of the atmosphere. Large quantities of H2O2 would then be adsorbed into the regolith, either as solid H2O2 "dust" or as re-evaporated vapor if the solid does not survive as it diffuses from its production region close to the surface. We suggest that this H2O2, or another superoxide processed from it in the surface, may be responsible for scavenging organic material from Mars. The presence of H2O2 in the surface could also accelerate the loss of methane from the atmosphere, thus requiring a larger source for maintaining a steady-state abundance of methane on Mars. The surface oxidants, together with storm electric fields and the harmful ultraviolet radiation that readily passes through the thin martian atmosphere, are likely to render the surface of Mars inhospitable to life as we know it.
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Affiliation(s)
- Sushil K Atreya
- Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Ann Arbor, Michigan, USA
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Farrell WM, Renno N, Delory GT, Cummer SA, Marshall JR. Integration of electrostatic and fluid dynamics within a dust devil. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002527] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Renno NO. MATADOR 2002: A pilot field experiment on convective plumes and dust devils. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2003je002219] [Citation(s) in RCA: 120] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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13
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Ferri F, Smith PH, Lemmon M, Rennó NO. Dust devils as observed by Mars Pathfinder. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2000je001421] [Citation(s) in RCA: 87] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Francesca Ferri
- Center of Studies and Activities for Space (CISAS), “G. Colombo,”; University of Padova; Padova Italy
| | - Peter H. Smith
- Lunar and Planetary Laboratory; University of Arizona; Tucson Arizona USA
| | - Mark Lemmon
- Texas A and M University; College Station Texas USA
| | - Nilton O. Rennó
- Department of Atmospheric, Oceanic and Space Sciences; University of Michigan; Ann Arbor Michigan USA
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Tratt DM. In situ measurement of dust devil dynamics: Toward a strategy for Mars. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002161] [Citation(s) in RCA: 44] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Merrison JP, Bertelsen P, Frandsen C, Gunnlaugsson P, Knudsen JM, Lunt S, Madsen MB, Mossin LA, Nielsen J, Nørnberg P, Rasmussen KR, Uggerhøj E. Simulation of the Martian dust aerosol at low wind speeds. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001807] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- J. P. Merrison
- Institute for Storage Ring Facilities; Aarhus University; Denmark
| | - P. Bertelsen
- Ørsted Laboratory; Niels Bohr Institute for Astronomy, Physics and Geophysics; Copenhagen Denmark
| | - C. Frandsen
- Ørsted Laboratory; Niels Bohr Institute for Astronomy, Physics and Geophysics; Copenhagen Denmark
| | - P. Gunnlaugsson
- Institute for Physics and Astronomy; Aarhus University; Denmark
| | - J. M. Knudsen
- Ørsted Laboratory; Niels Bohr Institute for Astronomy, Physics and Geophysics; Copenhagen Denmark
| | - S. Lunt
- Institute for Storage Ring Facilities; Aarhus University; Denmark
| | - M. B. Madsen
- Ørsted Laboratory; Niels Bohr Institute for Astronomy, Physics and Geophysics; Copenhagen Denmark
| | - L. A. Mossin
- Department of Earth Sciences; Aarhus University; Denmark
| | - J. Nielsen
- Institute for Physics and Astronomy; Aarhus University; Denmark
| | - P. Nørnberg
- Department of Earth Sciences; Aarhus University; Denmark
| | | | - E. Uggerhøj
- Institute for Storage Ring Facilities; Aarhus University; Denmark
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Newman CE, Lewis SR, Read PL, Forget F. Modeling the Martian dust cycle, 1. Representations of dust transport processes. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2002je001910] [Citation(s) in RCA: 166] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- Claire E. Newman
- Atmospheric, Oceanic and Planetary Physics, Department of Physics; Oxford University; Oxford UK
| | - Stephen R. Lewis
- Atmospheric, Oceanic and Planetary Physics, Department of Physics; Oxford University; Oxford UK
| | - Peter L. Read
- Atmospheric, Oceanic and Planetary Physics, Department of Physics; Oxford University; Oxford UK
| | - François Forget
- Laboratoire de Météorologie Dynamique du CNRS; Université Paris 6; Paris France
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Mustard JF, Cooper CD, Rifkin MK. Evidence for recent climate change on Mars from the identification of youthful near-surface ground ice. Nature 2001; 412:411-4. [PMID: 11473309 DOI: 10.1038/35086515] [Citation(s) in RCA: 451] [Impact Index Per Article: 19.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
Ground ice in the crust and soil may be one of the largest reservoirs of water on Mars. Near-surface ground ice is predicted to be stable at latitudes higher than 40 degrees (ref. 4), where a number of geomorphologic features indicative of viscous creep and hence ground ice have been observed. Mid-latitude soils have also been implicated as a water-ice reservoir, the capacity of which is predicted to vary on a 100,000-year timescale owing to orbitally driven variations in climate. It is uncertain, however, whether near-surface ground ice currently exists at these latitudes, and how it is changing with time. Here we report observational evidence for a mid-latitude reservoir of near-surface water ice occupying the pore space of soils. The thickness of the ice-occupied soil reservoir (1-10 m) and its distribution in the 30 degrees to 60 degrees latitude bands indicate a reservoir of (1.5-6.0) x 104 km3, equivalent to a global layer of water 10-40 cm thick. We infer that the reservoir was created during the last phase of high orbital obliquity less than 100,000 years ago, and is now being diminished.
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Affiliation(s)
- J F Mustard
- Department of Geological Sciences, Brown University, Providence, Rhode Island 02912, USA.
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