1
|
Characteristics of Dust Devils in Two Pre-Selected Landing Regions of the Tianwen-1 Mission—Comparing Observations and Predictions Using Numerical Model. REMOTE SENSING 2022. [DOI: 10.3390/rs14092117] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/04/2022]
Abstract
The spatial and temporal distribution of dust devils (DDs) in the two pre-selected landing regions (ZA and ZB) of the Tianwen-1 mission in southern Utopia Planitia have been investigated by using images from the Context Camera (CTX) of the Mars Reconnaissance Orbiter (MRO). From the images of the regions in 8 Martian years, no DD was found in ZA, while 77 DDs were found in ZB. The observed DDs are mainly distributed in the northeastern part of ZB. The temporal variation in the observed DDs shows a prominent two-peak pattern in their local early spring and late summer. The size and height of the observed DDs have also been evaluated from the images, and they show a similar temporal variation as the occurrence. To investigate the possible conditions pertinent to these observed patterns of DD distribution, some analysis based on the thermodynamic theory of heat engines was performed using the output of the Mars climate model, MarsWRF. The spatial and temporal distribution of the simulated DDs are generally consistent with the observation, with significantly more DDs in ZB. Analysis of the model results suggests that the spatial distributions of the predicted DDs are mainly related to the distribution of sensible heat flux, which, in turn, is mainly determined by the surface-to-air temperature difference. The difference in DDs between ZA and ZB (more DDs in ZB) is dominated by the difference in sensible heat flux, which, in turn, is mainly related to the spatial variation of surface albedo.
Collapse
|
2
|
Dundas CM, Becerra P, Byrne S, Chojnacki M, Daubar IJ, Diniega S, Hansen CJ, Herkenhoff KE, Landis ME, McEwen AS, Portyankina G, Valantinas A. Active Mars: A Dynamic World. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2021; 126:e2021JE006876. [PMID: 35845553 PMCID: PMC9285055 DOI: 10.1029/2021je006876] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/24/2021] [Revised: 06/17/2021] [Accepted: 06/21/2021] [Indexed: 06/15/2023]
Abstract
Mars exhibits diverse surface changes at all latitudes and all seasons. Active processes include impact cratering, aeolian sand and dust transport, a variety of slope processes, changes in polar ices, and diverse effects of seasonal CO2 frost. The extent of surface change has been surprising and indicates that the present climate is capable of reshaping the surface. Activity has important implications for the Amazonian history of Mars: understanding processes is a necessary step before we can understand their implications and variations over time.
Collapse
Affiliation(s)
- Colin M. Dundas
- U.S. Geological SurveyAstrogeology Science CenterFlagstaffAZUSA
| | | | - Shane Byrne
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | | | - Ingrid J. Daubar
- Department of Earth, Environmental, and Planetary SciencesBrown UniversityProvidenceRIUSA
| | - Serina Diniega
- Jet Propulsion Laboratory/California Institute of TechnologyPasadenaCAUSA
| | | | | | - Margaret E. Landis
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | | | - Ganna Portyankina
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | | |
Collapse
|
3
|
The Preliminary Study of Dust Devil Tracks in Southern Utopia Planitia, Landing Area of Tianwen-1 Mission. REMOTE SENSING 2021. [DOI: 10.3390/rs13132601] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/28/2022]
Abstract
China’s first Mars exploration mission (Tianwen-1) landed on the southern part of Mars’ Utopia Planitia on 15 May 2021. The Zhurong rover will focus on high-resolution and in situ observations of key areas on the surface of Mars. Dust devils (DDs) are heat-driven vortices that lift material from the surface and inject it into the atmosphere. The dark or bright surface lineaments left by DDs are called dust devil tracks (DDTs). Dust devils can clear dust from solar panels deposited by gusts and dust storms. Therefore, it is of importance to study the encounter rates of dust devils at the Tianwen-1 landing site for achieving the rover’s long-term scientific goals. Based on High Resolution Imaging Science Experiment (HiRISE) and Context Camera (CTX) images, 248 newly formed DDTs in 12 image pairs were firstly identified, and their lengths, widths, and direction in the study area were measured. The distribution of their width frequency follows a −2 differential power law. Secondly, DDT formation rates were computed and analyzed with the range of 0.00006 to 0.1275 ddt km−2 sol−1, mainly affected by factors such as seasons and dust storm occurrence. Thirdly, the solar panel clearing recurrence interval derived from the orbital data in our study area was calculated from ~980 to 166,700 sols. The dust storm occurrence probability at the Tianwen-1 landing area is less than 3%, and there is a special anti-dust coating on board the Zhurong rover. Thus, the Zhurong rover can be considered competent for scientific exploration.
Collapse
|
4
|
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.
Collapse
Affiliation(s)
- Brian Jackson
- Boise State University, Dept. of Physics 1910 University Drive, Boise ID 83725-1570
| |
Collapse
|
5
|
Raack J, Reiss D, Balme MR, Taj-Eddine K, Ori GG. In Situ Sampling of Relative Dust Devil Particle Loads and Their Vertical Grain Size Distributions. ASTROBIOLOGY 2018; 18:1305-1317. [PMID: 28422534 PMCID: PMC6205092 DOI: 10.1089/ast.2016.1544] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 06/01/2016] [Accepted: 12/29/2016] [Indexed: 06/07/2023]
Abstract
During a field campaign in the Sahara Desert in southern Morocco, spring 2012, we sampled the vertical grain size distribution of two active dust devils that exhibited different dimensions and intensities. With these in situ samples of grains in the vortices, it was possible to derive detailed vertical grain size distributions and measurements of the lifted relative particle load. Measurements of the two dust devils show that the majority of all lifted particles were only lifted within the first meter (∼46.5% and ∼61% of all particles; ∼76.5 wt % and ∼89 wt % of the relative particle load). Furthermore, ∼69% and ∼82% of all lifted sand grains occurred in the first meter of the dust devils, indicating the occurrence of "sand skirts." Both sampled dust devils were relatively small (∼15 m and ∼4-5 m in diameter) compared to dust devils in surrounding regions; nevertheless, measurements show that ∼58.5% to 73.5% of all lifted particles were small enough to go into suspension (<31 μm, depending on the used grain size classification). This relatively high amount represents only ∼0.05 to 0.15 wt % of the lifted particle load. Larger dust devils probably entrain larger amounts of fine-grained material into the atmosphere, which can have an influence on the climate. Furthermore, our results indicate that the composition of the surface, on which the dust devils evolved, also had an influence on the particle load composition of the dust devil vortices. The internal particle load structure of both sampled dust devils was comparable related to their vertical grain size distribution and relative particle load, although both dust devils differed in their dimensions and intensities. A general trend of decreasing grain sizes with height was also detected.
Collapse
Affiliation(s)
- Jan Raack
- School of Physical Science, Faculty of Science, Technology, Engineering & Mathematics (STEM), The Open University, Milton Keynes, UK
| | - Dennis Reiss
- Institut für Planetologie, Westfälische Wilhelms-Universität, Münster, Germany
| | - Matthew R. Balme
- School of Physical Science, Faculty of Science, Technology, Engineering & Mathematics (STEM), The Open University, Milton Keynes, UK
| | - Kamal Taj-Eddine
- Géologie et Géoinformatique, Faculté des Sciences Semlalia, Université Cadi Ayyad, Marrakech, Morocco
- Ibn Battuta Centre, Faculté des Sciences Semlalia, Université Cadi Ayyad, Marrakech, Morocco
| | - Gian Gabriele Ori
- Ibn Battuta Centre, Faculté des Sciences Semlalia, Université Cadi Ayyad, Marrakech, Morocco
- International Research School of Planetary Sciences, Università “G. D'Annunzio”, Pescara, Italy
| |
Collapse
|
6
|
Heavens N. Textured Dust Storm Activity in NE Amazonis-SW Arcadia, Mars: Phenomenology and Dynamical Interpretation. JOURNAL OF THE ATMOSPHERIC SCIENCES 2017; 74:1011-1037. [PMID: 32855571 PMCID: PMC7449148 DOI: 10.1175/jas-d-16-0211.1] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
Dust storms are Mars's most notable meteorological phenomenon, but many aspects of their structure and dynamics remain mysterious. The cloud-top appearance of dust storms in visible imagery varies on a continuum between diffuse/hazy and textured. Textured storms contain cellular structure and/or banding, which is thought to indicate active lifting within the storm. Some textured dust storms may contain the deep convection that generates the detached dust layers observed high in Mars's atmosphere. This study focuses on textured, local dust storms in a limited area within NE Amazonis and SW Arcadia Planitiae (25°-40° N,155°-165° W) using collocated observations by instruments on board the Mars Global Surveyor (MGS) and Mars Reconnaissance Orbiter (MRO) satellites. In northern fall and winter, this area frequently experiences dust storms with a previously unreported ruffled texture that resembles wide, mixed-layer rolls in the Earth's atmosphere, a resemblance that is supported by high resolution active sounding and passive radiometry in both the near and thermal infrared. These storms are mostly confined within the atmospheric boundary layer and are rarely sources of detached dust layers. The climatology and structure of these storms is thus consistent with an underlying driver of cold air advection events related to the passage of strong baroclinic waves. While the properties of the studied region may be ideal for detecting these structures and processes, the dynamics here are likely relevant to dust storm activity elsewhere on Mars.
Collapse
Affiliation(s)
- N.G. Heavens
- Department of Atmospheric and Planetary Sciences, Hampton University, Hampton, Virginia
| |
Collapse
|
7
|
Lorenz RD, Reiss D. Solar Panel Clearing Events, Dust Devil Tracks, and in-situ Vortex Detections on Mars. ICARUS 2015; 248:162-164. [PMID: 30705464 PMCID: PMC6350794 DOI: 10.1016/j.icarus.2014.10.034] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
Spirit rover solar array data, which if publicly-archived would provide a useful window on Mars meteorology, shows dust-clearing events coinciding with the onset of dust devil season in three Mars years. The recurrence interval of 100-700 days is consistent with the extrapolation of Pathfinder and Phoenix vortex encounters indicated by pressure drops of ~6-40 Pa (similar to laboratory measurements of dust lifting threshold) and with observed areas and rates of generation of dust devil tracks on Mars.
Collapse
Affiliation(s)
- Ralph D Lorenz
- Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
| | - Dennis Reiss
- Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany
| |
Collapse
|
8
|
Kok JF, Parteli EJR, Michaels TI, Karam DB. The physics of wind-blown sand and dust. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2012; 75:106901. [PMID: 22982806 DOI: 10.1088/0034-4885/75/10/106901] [Citation(s) in RCA: 158] [Impact Index Per Article: 13.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/12/2023]
Abstract
The transport of sand and dust by wind is a potent erosional force, creates sand dunes and ripples, and loads the atmosphere with suspended dust aerosols. This paper presents an extensive review of the physics of wind-blown sand and dust on Earth and Mars. Specifically, we review the physics of aeolian saltation, the formation and development of sand dunes and ripples, the physics of dust aerosol emission, the weather phenomena that trigger dust storms, and the lifting of dust by dust devils and other small-scale vortices. We also discuss the physics of wind-blown sand and dune formation on Venus and Titan.
Collapse
Affiliation(s)
- Jasper F Kok
- Department of Earth and Atmospheric Sciences, Cornell University, Ithaca, NY, USA.
| | | | | | | |
Collapse
|
9
|
Gheynani BT, Emami-Razavi M, Taylor PA. Thermophoresis and dust devils on the planet Mars. PHYSICAL REVIEW. E, STATISTICAL, NONLINEAR, AND SOFT MATTER PHYSICS 2011; 84:056305. [PMID: 22181496 DOI: 10.1103/physreve.84.056305] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/29/2011] [Revised: 08/08/2011] [Indexed: 05/31/2023]
Abstract
In the Martian atmosphere dust is abundant and is continuously replenished by the entrainment of materials and sediments from the surface of the planet. The sediment concentrations are particularly high and noticeable in whirlwinds, also known as dust devils. Assuming the thermophoresis force as the main driver of dust particles lifting from the surface, the dust process of the Martian atmosphere and its naturally formed dust devils are investigated for the northern polar region of the planet. Our simulated convective boundary layer shows that it may be unlikely that visible dust devils are formed only due to thermophoresis effects and some other lifting mechanisms are required.
Collapse
Affiliation(s)
- Babak T Gheynani
- Centre for Research in Earth and Space Science, York University, Toronto, Ontario, Canada
| | | | | |
Collapse
|
10
|
Tamppari LK, Bass D, Cantor B, Daubar I, Dickinson C, Fisher D, Fujii K, Gunnlauggson HP, Hudson TL, Kass D, Kleinböhl A, Komguem L, Lemmon MT, Mellon M, Moores J, Pankine A, Pathak J, Searls M, Seelos F, Smith MD, Smrekar S, Taylor P, Holstein-Rathlou C, Weng W, Whiteway J, Wolff M. Phoenix and MRO coordinated atmospheric measurements. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003415] [Citation(s) in RCA: 36] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
11
|
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]
|
12
|
Karunatillake S, Wray JJ, Squyres SW, Taylor GJ, Gasnault O, McLennan SM, Boynton W, El Maarry MR, Dohm JM. Chemically striking regions on Mars and Stealth revisited. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003303] [Citation(s) in RCA: 39] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|
13
|
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]
|
14
|
|
15
|
Malin MC, Bell JF, Cantor BA, Caplinger MA, Calvin WM, Clancy RT, Edgett KS, Edwards L, Haberle RM, James PB, Lee SW, Ravine MA, Thomas PC, Wolff MJ. Context Camera Investigation on board the Mars Reconnaissance Orbiter. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002808] [Citation(s) in RCA: 805] [Impact Index Per Article: 47.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
|