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McKeeby BE, Ramsey MS, Tai Udovicic CJ, Haberle C, Edwards CS. Quantifying Sub-Meter Surface Heterogeneity on Mars Using Off-Axis Thermal Emission Imaging System (THEMIS) Data. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2022; 9:e2022EA002430. [PMID: 36588669 PMCID: PMC9788145 DOI: 10.1029/2022ea002430] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 05/16/2022] [Revised: 07/26/2022] [Accepted: 08/03/2022] [Indexed: 06/17/2023]
Abstract
Surface heterogeneities below the spatial resolution of thermal infrared (TIR) instruments result in anisothermality and can produce emissivity spectra with negative slopes toward longer wavelengths. Sloped spectra arise from an incorrect assumption of either a uniform surface temperature or a maximum emissivity during the temperature-emissivity separation of radiance data. Surface roughness and lateral mixing of different sub-pixel surface units result in distinct spectral slopes with magnitudes proportional to the degree of temperature mixing. Routine Off-nadir Targeted Observations (ROTO) of the Thermal Emission Imaging Spectrometer (THEMIS) are used here for the first time to investigate anisothermality below the spatial resolution of THEMIS. The southern flank of Apollinaris Mons and regions within the Medusae Fossae Formation are studied using THEMIS ROTO data acquired just after local sunset. We observe a range of sloped TIR emission spectra dependent on the magnitude of temperature differences within a THEMIS pixel. Spectral slopes and wavelength-dependent brightness temperature differences are forward-modeled for a series of two-component surfaces of varying thermal inertia values. Our results imply that differing relative proportions of rocky and unconsolidated surface units are observed at each ROTO viewing geometry and suggest a local rock abundance six times greater than published results that rely on nadir data. High-resolution visible images of these regions indicate a mixture of surface units from boulders to dunes, providing credence to the model.
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Affiliation(s)
- B. E. McKeeby
- Department of Geology and Environmental ScienceUniversity of PittsburghPittsburghPAUSA
| | - M. S. Ramsey
- Department of Geology and Environmental ScienceUniversity of PittsburghPittsburghPAUSA
| | - C. J. Tai Udovicic
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - C. Haberle
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - C. S. Edwards
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
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Diurnal Variations of Water Ice in the Martian Atmosphere Observed by Mars Climate Sounder. REMOTE SENSING 2022. [DOI: 10.3390/rs14092235] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/05/2023]
Abstract
Simulation studies have proposed a significant thermal effect of water ice clouds on the Martian atmosphere and climate. However, previous studies focused more on seasonal variations but less on short-term changes. In this work, we used the MCS multi-local time data to investigate the water ice diurnal variations on Mars. We quantified its diurnal variations with amplitude and phase by applying the tidal fitting method to the water ice abundance. In addition, we found a close correlation (antiphase relation) between the thermal tide and water ice diurnal variations during the aphelion seasons that was not sensitive to both the background water ice and dust opacity but increased with the tidal amplitude. In the perihelion seasons, the antiphase relation was sensitive to the water ice and dust opacity, both affected by the dust storm activity. Finally, the statistic results suggested an unexpected low threshold of diurnal tide amplitude (2 to 3 K) for generating a relevant water ice diurnal variation, accounting for the ubiquitous water ice diurnal variations in the Martian atmosphere. These new observational results can help further understand the phase transition process between ice and vapor in the Martian atmosphere and better constrain the Martian global climate model in the future.
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Ruan T, Young RMB, Lewis SR, Montabone L, Valeanu A, Read PL. Assimilation of Both Column- and Layer-Integrated Dust Opacity Observations in the Martian Atmosphere. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2021; 8:e2021EA001869. [PMID: 35864913 PMCID: PMC9286790 DOI: 10.1029/2021ea001869] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 06/02/2021] [Revised: 11/10/2021] [Accepted: 11/30/2021] [Indexed: 06/15/2023]
Abstract
A new dust data assimilation scheme has been developed for the UK version of the Laboratoire de Météorologie Dynamique Martian General Circulation Model. The Analysis Correction scheme (adapted from the UK Met Office) is applied with active dust lifting and transport to analyze measurements of temperature, and both column-integrated dust optical depth (CIDO), τ ref (rescaled to a reference level), and layer-integrated dust opacity (LIDO). The results are shown to converge to the assimilated observations, but assimilating either of the dust observation types separately does not produce the best analysis. The most effective dust assimilation is found to require both CIDO (from Mars Odyssey/THEMIS) and LIDO observations, especially for Mars Climate Sounder data that does not access levels close to the surface. The resulting full reanalysis improves the agreement with both in-sample assimilated CIDO and LIDO data and independent observations from outside the assimilated data set. It is thus able to capture previously elusive details of the dust vertical distribution, including elevated detached dust layers that have not been captured in previous reanalyzes. Verification of this reanalysis has been carried out under both clear and dusty atmospheric conditions during Mars Years 28 and 29, using both in-sample and out of sample observations from orbital remote sensing and contemporaneous surface measurements of dust opacity from the Spirit and Opportunity landers. The reanalysis was also compared with a recent version of the Mars Climate Database (MCD v5), demonstrating generally good agreement though with some systematic differences in both time mean fields and day-to-day variability.
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Affiliation(s)
- Tao Ruan
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
| | - R. M. B. Young
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
- Department of Physics & National Space Science and Technology CenterUAE UniversityAl AinUnited Arab Emirates
| | - S. R. Lewis
- School of Physical SciencesThe Open UniversityMilton KeynesUK
| | - L. Montabone
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
- Space Science InstituteBoulderCOUSA
| | - A. Valeanu
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
| | - P. L. Read
- Department of PhysicsAtmospheric, Oceanic and Planetary PhysicsUniversity of OxfordClarendon LaboratoryOxfordUK
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Smith MD. Local time variation of water ice clouds on Mars as observed by THEMIS. ICARUS 2019; 333:273-282. [PMID: 31708590 PMCID: PMC6839708 DOI: 10.1016/j.icarus.2019.06.009] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
The move of the Odyssey spacecraft during Mars Years 31 and 32 to an orbit with local time near 7:00 AM and PM has enabled the systematic retrieval of water ice cloud optical depth using THEMIS thermal infrared images at a time of day not accessible from Mars Global Surveyor, Mars Reconnaissance Orbiter, or previous Odyssey observations. Because water ice clouds form by condensation, relatively small changes in atmospheric temperature can cause clouds to form or sublimate quickly, and there can be large changes in water ice cloud optical depth over the course of a day. Retrievals of water ice cloud optical depth using THEMIS observations show significant differences in cloud locations and optical depth as a function of local time and season. Cloud optical depth generally increases from the earliest (14:30) to latest (19:30) observations. During the aphelion season the increase from afternoon to evening is primarily associated with the thickening of existing clouds, while during the equinoctial and perihelion seasons there is a proportionally greater increase associated with the formation of clouds in the evening at locations where clouds were not present during the afternoon.
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Affiliation(s)
- Michael D. Smith
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States
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Moores JE, Lemmon MT, Smith PH, Komguem L, Whiteway JA. Atmospheric dynamics at the Phoenix landing site as seen by the Surface Stereo Imager. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003409] [Citation(s) in RCA: 23] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Edwards CS, Bandfield JL, Christensen PR, Fergason RL. Global distribution of bedrock exposures on Mars using THEMIS high-resolution thermal inertia. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003363] [Citation(s) in RCA: 65] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Smith MD, Wolff MJ, Clancy RT, Murchie SL. Compact Reconnaissance Imaging Spectrometer observations of water vapor and carbon monoxide. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003288] [Citation(s) in RCA: 118] [Impact Index Per Article: 7.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Lee C, Lawson WG, Richardson MI, Heavens NG, Kleinböhl A, Banfield D, McCleese DJ, Zurek R, Kass D, Schofield JT, Leovy CB, Taylor FW, Toigo AD. Thermal Tides in the Martian Middle Atmosphere as Seen by the Mars Climate Sounder. ACTA ACUST UNITED AC 2009; 114. [PMID: 27630378 DOI: 10.1029/2008je003285] [Citation(s) in RCA: 75] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
The first systematic observations of the middle atmosphere of Mars (35km-80km) with the Mars Climate Sounder (MCS) show dramatic patterns of diurnal thermal variation, evident in retrievals of temperature and water ice opacity. At the time of writing, the dataset of MCS limb retrievals is sufficient for spectral analysis within a limited range of latitudes and seasons. This analysis shows that these thermal variations are almost exclusively associated with a diurnal thermal tide. Using a Martian General Circulation Model to extend our analysis we show that the diurnal thermal tide dominates these patterns for all latitudes and all seasons.
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Affiliation(s)
- C Lee
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - W G Lawson
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - M I Richardson
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - N G Heavens
- Division of Geological and Planetary Sciences, California Institute of Technology
| | - A Kleinböhl
- Jet Propulsion Laboratory, California Institute of Technology
| | - D Banfield
- Department of Astronomy, Cornell University
| | - D J McCleese
- Jet Propulsion Laboratory, California Institute of Technology
| | - R Zurek
- Jet Propulsion Laboratory, California Institute of Technology
| | - D Kass
- Jet Propulsion Laboratory, California Institute of Technology
| | - J T Schofield
- Jet Propulsion Laboratory, California Institute of Technology
| | - C B Leovy
- Department of Atmospheric Sciences, University of Washington
| | - F W Taylor
- Department of Physics, University of Oxford
| | - A D Toigo
- Department of Astronomy, Cornell University
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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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Langevin Y, Bibring JP, Montmessin F, Forget F, Vincendon M, Douté S, Poulet F, Gondet B. Observations of the south seasonal cap of Mars during recession in 2004-2006 by the OMEGA visible/near-infrared imaging spectrometer on board Mars Express. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002841] [Citation(s) in RCA: 104] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- Y. Langevin
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - J.-P. Bibring
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - F. Montmessin
- Service d'Aéronomie; CNRS/Université Pierre et Marie Curie; Verrières-le-Buisson France
| | - F. Forget
- Laboratoire de Météorologie Dynamique; CNRS/Université Pierre et Marie Curie; Paris France
| | - M. Vincendon
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - S. Douté
- Laboratoire de Planétologie de Grenoble; CNRS/Université Joseph Fourier; Grenoble France
| | - F. Poulet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
| | - B. Gondet
- Institut d'Astrophysique Spatiale; CNRS/Université Paris Sud; Orsay France
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Murchie S, Arvidson R, Bedini P, Beisser K, Bibring JP, Bishop J, Boldt J, Cavender P, Choo T, Clancy RT, Darlington EH, Des Marais D, Espiritu R, Fort D, Green R, Guinness E, Hayes J, Hash C, Heffernan K, Hemmler J, Heyler G, Humm D, Hutcheson J, Izenberg N, Lee R, Lees J, Lohr D, Malaret E, Martin T, McGovern JA, McGuire P, Morris R, Mustard J, Pelkey S, Rhodes E, Robinson M, Roush T, Schaefer E, Seagrave G, Seelos F, Silverglate P, Slavney S, Smith M, Shyong WJ, Strohbehn K, Taylor H, Thompson P, Tossman B, Wirzburger M, Wolff M. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO). ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002682] [Citation(s) in RCA: 666] [Impact Index Per Article: 39.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Smith MD, Wolff MJ, Spanovich N, Ghosh A, Banfield D, Christensen PR, Landis GA, Squyres SW. One Martian year of atmospheric observations using MER Mini-TES. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002770] [Citation(s) in RCA: 127] [Impact Index Per Article: 7.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
| | | | | | | | - Don Banfield
- Department of Astronomy; Cornell University; Ithaca New York USA
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Noe Dobrea EZ, Bell JF, McConnochie TH, Malin M. Analysis of a spectrally unique deposit in the dissected Noachian terrain of Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002431] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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14
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Bandfield JL. Atmospheric correction and surface spectral unit mapping using Thermal Emission Imaging System data. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002289] [Citation(s) in RCA: 80] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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