1
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Sánchez‐Lavega A, del Rio‐Gaztelurrutia T, Hueso R, Juárez MDLT, Martínez GM, Harri A, Genzer M, Hieta M, Polkko J, Rodríguez‐Manfredi JA, Lemmon MT, Pla‐García J, Toledo D, Vicente‐Retortillo A, Viúdez‐Moreiras D, Munguira A, Tamppari LK, Newman C, Gómez‐Elvira J, Guzewich S, Bertrand T, Apéstigue V, Arruego I, Wolff M, Banfield D, Jaakonaho I, Mäkinen T. Mars 2020 Perseverance Rover Studies of the Martian Atmosphere Over Jezero From Pressure Measurements. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2023; 128:e2022JE007480. [PMID: 37034458 PMCID: PMC10078360 DOI: 10.1029/2022je007480] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/10/2022] [Revised: 10/05/2022] [Accepted: 10/24/2022] [Indexed: 06/16/2023]
Abstract
The pressure sensors on Mars rover Perseverance measure the pressure field in the Jezero crater on regular hourly basis starting in sol 15 after landing. The present study extends up to sol 460 encompassing the range of solar longitudes from L s ∼ 13°-241° (Martian Year (MY) 36). The data show the changing daily pressure cycle, the sol-to-sol seasonal evolution of the mean pressure field driven by the CO2 sublimation and deposition cycle at the poles, the characterization of up to six components of the atmospheric tides and their relationship to dust content in the atmosphere. They also show the presence of wave disturbances with periods 2-5 sols, exploring their baroclinic nature, short period oscillations (mainly at night-time) in the range 8-24 min that we interpret as internal gravity waves, transient pressure drops with duration ∼1-150 s produced by vortices, and rapid turbulent fluctuations. We also analyze the effects on pressure measurements produced by a regional dust storm over Jezero at L s ∼ 155°.
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Affiliation(s)
| | | | | | | | | | - A.‐M. Harri
- Finnish Meteorological InstituteHelsinkiFinland
| | - M. Genzer
- Finnish Meteorological InstituteHelsinkiFinland
| | - M. Hieta
- Finnish Meteorological InstituteHelsinkiFinland
| | - J. Polkko
- Finnish Meteorological InstituteHelsinkiFinland
| | | | | | | | - D. Toledo
- Centro de Astrobiología (INTA‐CSIC)MadridSpain
| | | | | | | | - L. K. Tamppari
- Jet Propulsion Laboratory/California Institute of TechnologyPasadenaCAUSA
| | | | | | - S. Guzewich
- NASA Goddard Space Flight CenterGreenbeltMDUSA
| | | | - V. Apéstigue
- Instituto Nacional de Técnica AeroespacialINTAMadridSpain
| | - I. Arruego
- Instituto Nacional de Técnica AeroespacialINTAMadridSpain
| | - M. Wolff
- Space Science InstituteBrookfieldWIUSA
| | | | | | - T. Mäkinen
- Finnish Meteorological InstituteHelsinkiFinland
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2
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Lemmon MT, Smith MD, Viudez‐Moreiras D, de la Torre‐Juarez M, Vicente‐Retortillo A, Munguira A, Sanchez‐Lavega A, Hueso R, Martinez G, Chide B, Sullivan R, Toledo D, Tamppari L, Bertrand T, Bell JF, Newman C, Baker M, Banfield D, Rodriguez‐Manfredi JA, Maki JN, Apestigue V. Dust, Sand, and Winds Within an Active Martian Storm in Jezero Crater. GEOPHYSICAL RESEARCH LETTERS 2022; 49:e2022GL100126. [PMID: 36245893 PMCID: PMC9540647 DOI: 10.1029/2022gl100126] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 06/20/2022] [Revised: 08/19/2022] [Accepted: 08/22/2022] [Indexed: 06/16/2023]
Abstract
Rovers and landers on Mars have experienced local, regional, and planetary-scale dust storms. However, in situ documentation of active lifting within storms has remained elusive. Over 5-11 January 2022 (LS 153°-156°), a dust storm passed over the Perseverance rover site. Peak visible optical depth was ∼2, and visibility across the crater was briefly reduced. Pressure amplitudes and temperatures responded to the storm. Winds up to 20 m s-1 rotated around the site before the wind sensor was damaged. The rover imaged 21 dust-lifting events-gusts and dust devils-in one 25-min period, and at least three events mobilized sediment near the rover. Rover tracks and drill cuttings were extensively modified, and debris was moved onto the rover deck. Migration of small ripples was seen, but there was no large-scale change in undisturbed areas. This work presents an overview of observations and initial results from the study of the storm.
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Affiliation(s)
| | - M. D. Smith
- NASA Goddard Space Flight CenterGreenbeltMDUSA
| | | | | | | | - A. Munguira
- Física Aplicada, Escuela de Ingeniería de BilbaoUPV/EHUBilbaoSpain
| | | | - R. Hueso
- Física Aplicada, Escuela de Ingeniería de BilbaoUPV/EHUBilbaoSpain
| | | | - B. Chide
- Space and Planetary Exploration TeamLos Alamos National LaboratoryLos AlamosNMUSA
| | | | - D. Toledo
- Instituto Nacional de Técnica AerospacialMadridSpain
| | - L. Tamppari
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | | | - M. Baker
- Smithsonian National Air and Space MuseumWashingtonDCUSA
| | | | | | - J. N. Maki
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - V. Apestigue
- Instituto Nacional de Técnica AerospacialMadridSpain
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3
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Abstract
Recurring Slope Lineae (RSL) on Mars have been enigmatic since their discovery; their behavior resembles a seeping liquid but sources of water remain puzzling. This work demonstrates that the properties of RSL are consistent with observed behaviors of Martian and terrestrial aeolian processes. Specifically, RSL are well-explained as flows of sand that remove a thin coating of dust. Observed RSL properties are supportive of or consistent with this model, which requires no liquid water or other exotic processes, but rather indicates seasonal aeolian behavior. These settings and behaviors resemble features observed by rovers and also explain the occurrence of many slope lineae on Mars that do not meet the strict definition of RSL. This indicates that RSL can be explained simply as aeolian features. Other processes may add complexities just as they could modify the behavior of any sand dune.
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Affiliation(s)
- Colin M. Dundas
- U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA
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4
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Streeter PM, Lewis SR, Patel MR, Holmes JA, Kass DM. Surface Warming During the 2018/Mars Year 34 Global Dust Storm. GEOPHYSICAL RESEARCH LETTERS 2020; 47:e2019GL083936. [PMID: 32713983 PMCID: PMC7375149 DOI: 10.1029/2019gl083936] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/31/2019] [Revised: 08/29/2019] [Accepted: 09/02/2019] [Indexed: 06/11/2023]
Abstract
The impact of Mars's 2018 Global Dust Storm (GDS) on surface and near-surface air temperatures was investigated using an assimilation of Mars Climate Sounder observations. Rather than simply resulting in cooling everywhere from solar absorption (average surface radiative flux fell 26 W/m2), the globally averaged result was a 0.9-K surface warming. These diurnally averaged surface temperature changes had a novel, highly nonuniform spatial structure, with up to 16-K cooling/19-K warming. Net warming occurred in low thermal inertia regions, where rapid nighttime radiative cooling was compensated by increased longwave emission and scattering. This caused strong nightside warming, outweighing dayside cooling. The reduced surface-air temperature gradient closely coupled surface and air temperatures, even causing local dayside air warming. Results show good agreement with Mars Climate Sounder surface temperature retrievals. Comparisons with the 2001 GDS and free-running simulations show that GDS spatial structure is crucial in determining global surface temperature effects.
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Affiliation(s)
| | | | - Manish R. Patel
- School of Physical SciencesThe Open UniversityMilton KeynesUK
- Space Science and Technology DepartmentScience and Technology Facilities Council, Rutherford Appleton LaboratoryDidcotUK
| | - James A. Holmes
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - David M. Kass
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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5
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Viúdez-Moreiras D, Newman CE, de la Torre M, Martínez G, Guzewich S, Lemmon M, Pla-García J, Smith MD, Harri AM, Genzer M, Vicente-Retortillo A, Lepinette A, Rodriguez-Manfredi JA, Vasavada AR, Gómez-Elvira J. Effects of the MY34/2018 Global Dust Storm as Measured by MSL REMS in Gale Crater. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2019; 124:1899-1912. [PMID: 31534881 PMCID: PMC6750032 DOI: 10.1029/2019je005985] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/29/2019] [Accepted: 06/19/2019] [Indexed: 05/28/2023]
Abstract
The Rover Environmental Monitoring Station (REMS) instrument that is onboard NASA's Mars Science Laboratory (MSL) Curiosity rover. REMS has been measuring surface pressure, air and ground brightness temperature, relative humidity, and UV irradiance since MSL's landing in 2012. In Mars Year (MY) 34 (2018) a global dust storm reached Gale Crater at Ls ~190°. REMS offers a unique opportunity to better understand the impact of a global dust storm on local environmental conditions, which complements previous observations by the Viking landers and Mars Exploration Rovers. All atmospheric variables measured by REMS are strongly affected albeit at different times. During the onset phase, the daily maximum UV radiation decreased by 90% between sols 2075 (opacity ~1) and 2085 (opacity ~8.5). The diurnal range in ground and air temperatures decreased by 35K and 56K, respectively, with also a diurnal-average decrease of ~2K and 4K respectively. The maximum relative humidity, which occurs right before sunrise, decreased to below 5%, compared with pre-storm values of up to 29%, due to the warmer air temperatures at night while the inferred water vapor abundance suggests an increase during the storm. Between sols 2085 and 2130, the typical nighttime stable inversion layer was absent near the surface as ground temperatures remained warmer than near-surface air temperatures. Finally, the frequency-domain behavior of the diurnal pressure cycle shows a strong increase in the strength of the semidiurnal and terdiurnal modes peaking after the local opacity maximum, also suggesting differences in the dust abundance inside and outside Gale.
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Affiliation(s)
- D Viúdez-Moreiras
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - C E Newman
- Aeolis Research, 600 N. Rosemead Ave., Suite 205, Pasadena, CA 91106, USA
| | - M de la Torre
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - G Martínez
- University of Michigan, Ann Arbor, Michigan, USA
| | - S Guzewich
- NASA Goddard Spaceflight Center, Greenbelt, MD, USA
| | - M Lemmon
- Space Science Institute, College Station, TX 77843 USA
| | - J Pla-García
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - M D Smith
- NASA Goddard Spaceflight Center, Greenbelt, MD, USA
| | - A-M Harri
- Earth Observation, Finnish Meteorological Institute, Erik Palménin aukio, Helsinki, Finland
| | - M Genzer
- Earth Observation, Finnish Meteorological Institute, Erik Palménin aukio, Helsinki, Finland
| | | | - A Lepinette
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - J A Rodriguez-Manfredi
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
| | - A R Vasavada
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
| | - J Gómez-Elvira
- Centro de Astrobiología (CSIC-INTA) & Spanish National Institute for Aerospace Technology (INTA), Torrejón de Ardoz, Madrid, Spain
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6
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Ojha L, Lewis K, Karunatillake S, Schmidt M. The Medusae Fossae Formation as the single largest source of dust on Mars. Nat Commun 2018; 9:2867. [PMID: 30030425 PMCID: PMC6054634 DOI: 10.1038/s41467-018-05291-5] [Citation(s) in RCA: 23] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/29/2017] [Accepted: 06/26/2018] [Indexed: 11/09/2022] Open
Abstract
Transport of fine-grained dust is one of the most widespread sedimentary processes occurring on Mars today. In the present climate, eolian abrasion and deflation of rocks are likely the most pervasive and active dust-forming mechanism. Martian dust is globally enriched in S and Cl and has a distinct mean S:Cl ratio. Here we identify a potential source region for Martian dust based on analysis of elemental abundance data. We show that a large sedimentary unit called the Medusae Fossae Formation (MFF) has the highest abundance of S and Cl, and provides the best chemical match to surface measurements of Martian dust. Based on volume estimates of the eroded materials from the MFF, along with the enrichment of elemental S and Cl, and overall geochemical similarity, we propose that long-term deflation of the MFF has significantly contributed to the global Martian dust reservoir.
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Affiliation(s)
- Lujendra Ojha
- Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, 21218, USA.
| | - Kevin Lewis
- Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, 21218, USA
| | - Suniti Karunatillake
- Department of Geology and Geophysics, Louisiana State University, Baton Rouge, LA, 70803, USA
| | - Mariek Schmidt
- Department of Earth Sciences, Brock University, St. Catharines, ON, L2S 3A1, Canada
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7
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Haberle RM, Pollack JB, Barnes JR, Zurek RW, Leovy CB, Murphy JR, Lee H, Schaeffer J. Mars atmospheric dynamics as simulated by the NASA Ames General Circulation Model: 1. The zonal-mean circulation. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/92je02946] [Citation(s) in RCA: 265] [Impact Index Per Article: 22.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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8
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Zurek RW, Martin LJ. Interannual variability of planet-encircling dust storms on Mars. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/92je02936] [Citation(s) in RCA: 132] [Impact Index Per Article: 11.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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9
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Guinness EA. Spectral properties (0.40 to 0.75 microns) of soils exposed at the Viking 1 landing site. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb086ib09p07983] [Citation(s) in RCA: 20] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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10
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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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11
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Strausberg MJ. Observations of the initiation and evolution of the 2001 Mars global dust storm. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002361] [Citation(s) in RCA: 93] [Impact Index Per Article: 4.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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12
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Golombek MP, Bridges NT. Erosion rates on Mars and implications for climate change: Constraints from the Pathfinder landing site. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001043] [Citation(s) in RCA: 146] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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13
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Seiff A, Tillman JE, Murphy JR, Schofield JT, Crisp D, Barnes JR, LaBaw C, Mahoney C, Mihalov JD, Wilson GR, Haberle R. The atmosphere structure and meteorology instrument on the Mars Pathfinder lander. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/96je03320] [Citation(s) in RCA: 56] [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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14
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Santee ML, Crisp D. Diagnostic calculations of the circulation in the Martian atmosphere. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je03207] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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15
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Martin TZ, Richardson MI. New dust opacity mapping from Viking infrared thermal mapper data. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93je01044] [Citation(s) in RCA: 60] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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16
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Tillman JE, Johnson NC, Guttorp P, Percival DB. The Martian annual atmospheric pressure cycle: Years without great dust storms. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93je01084] [Citation(s) in RCA: 95] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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McCleese DJ, Haskins RD, Schofield JT, Zurek RW, Leovy CB, Paige DA, Taylor FW. Atmosphere and climate studies of Mars using the Mars Observer pressure modulator infrared radiometer. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je00539] [Citation(s) in RCA: 24] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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18
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19
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Murphy JR, Leovy CB, Tillman JE. Observations of Martian surface winds at the Viking Lander 1 Site. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14555] [Citation(s) in RCA: 58] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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20
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Murphy JR, Toon OB, Haberle RM, Pollack JB. Numerical simulations of the decay of Martian global dust storms. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14629] [Citation(s) in RCA: 42] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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21
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Tillman JE. Mars global atmospheric oscillations: Annually synchronized, transient normal-mode oscillations and the triggering of global dust storms. ACTA ACUST UNITED AC 1988. [DOI: 10.1029/jd093id08p09433] [Citation(s) in RCA: 104] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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22
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Morris RV, Lauer HV, Lawson CA, Gibson EK, Nace GA, Stewart C. Spectral and other physicochemical properties of submicron powders of hematite (alpha-Fe2O3), maghemite (gamma-Fe2O3), magnetite (Fe3O4), goethite (alpha-FeOOH), and lepidocrocite (gamma-FeOOH). JOURNAL OF GEOPHYSICAL RESEARCH 1985; 90:3126-44. [PMID: 11542003 DOI: 10.1029/jb090ib04p03126] [Citation(s) in RCA: 112] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Abstract
Spectral and other physicochemical properties were determined for a suite of submicron powders of hematite (alpha-Fe2O3), maghemite (gamma-Fe2O3), magnetite (Fe3O4), goethite (alpha-FeOOH), and lepidocrocite (gamma-FeOOH). The spectral reflectivity measurements were made between 0.35 and 2.20 micrograms over the temperature interval between about -110 degrees and 20 degrees C. Other physicochemical properties determined were mean particle diameter, particle shape, chemical composition, crystallographic phase, magnetic properties, and Mossbauer properties. Only the magnetite powders have significant departures from the stoichiometric phase; they are actually cation-deficient magnetites having down to about 18.0 wt % FeO as compared with 31.0 wt % FeO for stoichiometric magnetite. A structured absorption edge due to crystal field transitions and extending from weak absorption in the near-IR to intense absorption in the near-UV is characteristic of the ferric oxides and oxyhydroxides and is responsible for their intense color. Particularly for hematite, the number and position of the spectral features are consistent with significant splitting of the degenerate cubic levels by noncubic components of the crystal field. The position of the crystal-field band at lowest energy, assigned to the envelope of the components of the split cubic 4T1 level, is near 0.86, 0.91, 0.92, and 0.98 microgram at room temperature for hematite, goethite, maghemite, and lepidocrocite, respectively. Comparison with Mossbauer data suggests covalent character increases sequentially through the aforementioned series. The positions of the spectra features are relatively independent of temperature down to about -110 degrees C. The maximum shifts observed were on the order of about 0.02 microgram shortward for the ferric oxyhydroxides. Variations in the magnitude of the reflectivity of the hematite powders as a function of mean particle diameter are consistent with scattering theory. The absorption strength of the crystal-field bands increases with increasing mean particle diameter over the range 0.1-0.8 micrometer; visually this corresponds to a change in color from orange to deep purple. The position of the split cubic 4T1 band shifts longward by about 0.02 micrometer with decreasing mean particle diameter over the same range; this trend is consistent with wavelength-dependent scattering. The cation-deficient magnetite powders are very strong absorbers throughout the near-UV, visible and near-IR; their spectral properties are independent of temperature between about -110 and 20 degrees C.
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Affiliation(s)
- R V Morris
- Experimental Planetology Branch, NASA Johnson Space Center, Houston, Texas, USA
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23
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24
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Kahn R. The spatial and seasonal distribution of Martian clouds and some meteorological implications. ACTA ACUST UNITED AC 1984. [DOI: 10.1029/ja089ia08p06671] [Citation(s) in RCA: 79] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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25
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26
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27
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Huguenin RL, Clifford SM. Remote sensing evidence for regolith water vapor sources on Mars. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/jb087ib12p10227] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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28
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James PB, North GR. The seasonal CO2cycle on Mars: An application of an energy balance climate model. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/jb087ib12p10271] [Citation(s) in RCA: 59] [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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29
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Guinness EA, Leff CE, Arvidson RE. Two Mars years of surface changes seen at the Viking landing sites. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/jb087ib12p10051] [Citation(s) in RCA: 27] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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30
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31
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Lee SW, Thomas PC, Veverka J. Wind streaks in Tharsis and Elysium: Implications for sediment transport by slope winds. ACTA ACUST UNITED AC 1982. [DOI: 10.1029/jb087ib12p10025] [Citation(s) in RCA: 37] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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32
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Ryan JA, Sharman RD. Two major dust storms, one Mars year apart: Comparison from Viking data. ACTA ACUST UNITED AC 1981. [DOI: 10.1029/jc086ic04p03247] [Citation(s) in RCA: 36] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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33
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Abstract
Physical and chemical considerations permit the division of the near-surface regolith on Mars into at least six zones of distinct microenvironments. The zones are euphotic, duricrust/peds, tempofrost, permafrost, endolithic, and interfacial/transitional. Microenvironments vary significantly in temperature extremes, mean temperature, salt content, relative pressure of water vapor, UV and visible light irradiance, and exposure to ionizing radiation events (100 Mrad) and oxidative molecular species. From what is known of the chemistry of the atmosphere and regolith fines (soil), limits upon the aqueous chemistry of soil pastes may be estimated. Heat of wetting could reach 45 cal/g dry soil; initial pH is indeterminate between 1 and 10; ionic strength and salinity are predicted to be extremely high; freezing point depression is inadequate to provide quantities of liquid water except in special cases. The prospects for biotic survival are grim by terrestrial standards, but the extremes of biological resiliency are inaccessible to evaluation. Second-generation in situ experiments which will better define Martian microenvironments are clearly possible. Antarctic dry valleys are approximations to Martian conditions, but deviate significantly by at least half-a-dozen criteria.
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34
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Jones KL, Arvidson RE, Guinness EA, Bragg SL, Wall SD, Carlston CE, Pidek DG. One Mars Year: Viking Lander Imaging Observations. Science 1979; 204:799-806. [PMID: 17730507 DOI: 10.1126/science.204.4395.799] [Citation(s) in RCA: 92] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Throughout the complete Mars year during which they have been on the planet, the imaging systems aboard the two Viking landers have documented a variety of surface changes. Surface condensates, consisting of both solid H(2)O and CO(2), formed at the Viking 2 lander site during the winter. Additional observations suggest that surface erosion rates due to dust redistribution may be substantially less than those predicted on the basis of pre-Viking observations. The Viking 1 lander will continue to acquire and transmit a predetermined sequence of imaging and meteorology data as long as it is operative.
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35
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Peterfreund AR, Kieffer HH. Thermal infrared properties of the Martian atmosphere: 3. Local dust clouds. ACTA ACUST UNITED AC 1979. [DOI: 10.1029/jb084ib06p02853] [Citation(s) in RCA: 61] [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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