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Viúdez‐Moreiras D, de la Torre M, Gómez‐Elvira J, Lorenz RD, Apéstigue V, Guzewich S, Mischna M, Sullivan R, Herkenhoff K, Toledo D, Lemmon M, Smith M, Newman CE, Sánchez‐Lavega A, Rodríguez‐Manfredi JA, Richardson M, Hueso R, Harri AM, Tamppari L, Arruego I, Bell J. Winds at the Mars 2020 Landing Site. 2. Wind Variability and Turbulence. J Geophys Res Planets 2022; 127:e2022JE007523. [PMID: 37033152 PMCID: PMC10078282 DOI: 10.1029/2022je007523] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 08/06/2022] [Revised: 11/18/2022] [Accepted: 11/29/2022] [Indexed: 06/19/2023]
Abstract
Wind speeds measured by the Mars 2020 Perseverance rover in Jezero crater were fitted as a Weibull distribution. InSight wind data acquired in Elysium Planitia were also used to contextualize observations. Jezero winds were found to be much calmer on average than in previous landing sites, despite the intense aeolian activity observed. However, a great influence of turbulence and wave activity was observed in the wind speed variations, thus driving the probability of reaching the highest wind speeds at Jezero, instead of sustained winds driven by local, regional, or large-scale circulation. The power spectral density of wind speed fluctuations follows a power-law, whose slope deviates depending on the time of day from that predicted considering homogeneous and isotropic turbulence. Daytime wave activity is related to convection cells and smaller eddies in the boundary layer, advected over the crater. The signature of convection cells was also found during dust storm conditions, when prevailing winds were consistent with a tidal drive. Nighttime fluctuations were also intense, suggesting strong mechanical turbulence. Convective vortices were usually involved in rapid wind fluctuations and extreme winds, with variations peaking at 9.2 times the background winds. Transient high wind events by vortex-passages, turbulence, and wave activity could be driving aeolian activity at Jezero. We report the detection of a strong dust cloud of 0.75-1.5 km in length passing over the rover. The observed aeolian activity had major implications for instrumentation, with the wind sensor suffering damage throughout the mission, probably due to flying debris advected by winds.
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Affiliation(s)
- D. Viúdez‐Moreiras
- Centro de Astrobiología (CAB, CSIC‐INTA) and National Institute for Aerospace Technology (INTA)MadridSpain
| | - M. de la Torre
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Gómez‐Elvira
- National Institute for Aerospace Technology (INTA)MadridSpain
| | | | - V. Apéstigue
- National Institute for Aerospace Technology (INTA)MadridSpain
| | - S. Guzewich
- NASA Goddard Spaceflight CenterGreenbeltMDUSA
| | - M. Mischna
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | - D. Toledo
- National Institute for Aerospace Technology (INTA)MadridSpain
| | - M. Lemmon
- Space Science InstituteCollege StationTXUSA
| | - M. Smith
- NASA Goddard Spaceflight CenterGreenbeltMDUSA
| | | | | | - J. A. Rodríguez‐Manfredi
- Centro de Astrobiología (CAB, CSIC‐INTA) and National Institute for Aerospace Technology (INTA)MadridSpain
| | | | - R. Hueso
- Universidad del País Vasco (UPV/EHU)BilbaoSpain
| | - A. M. Harri
- Finnish Meteorological InstituteHelsinkiFinland
| | - L. Tamppari
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - I. Arruego
- National Institute for Aerospace Technology (INTA)MadridSpain
| | - J. Bell
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
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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. Geophys Res Lett 2022; 49:e2022GL100126. [PMID: 36245893 PMCID: PMC9540647 DOI: 10.1029/2022gl100126] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [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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Lemmon MT, Toledo D, Apestigue V, Arruego I, Wolff MJ, Patel P, Guzewich S, Colaprete A, Vicente‐Retortillo Á, Tamppari L, Montmessin F, de la Torre Juarez M, Maki J, McConnochie T, Brown A, Bell JF. Hexagonal Prisms Form in Water-Ice Clouds on Mars, Producing Halo Displays Seen by Perseverance Rover. Geophys Res Lett 2022; 49:e2022GL099776. [PMID: 36245894 PMCID: PMC9539710 DOI: 10.1029/2022gl099776] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/31/2022] [Revised: 08/18/2022] [Accepted: 08/22/2022] [Indexed: 06/16/2023]
Abstract
Observations by several cameras on the Perseverance rover showed a 22° scattering halo around the Sun over several hours during northern midsummer (solar longitude 142°). Such a halo has not previously been seen beyond Earth. The halo occurred during the aphelion cloud belt season and the cloudiest time yet observed from the Perseverance site. The halo required crystalline water-ice cloud particles in the form of hexagonal columns large enough for refraction to be significant, at least 11 μm in diameter and length. From a possible 40-50 km altitude, and over the 3.3 hr duration of the halo, particles could have fallen 3-12 km, causing downward transport of water and dust. Halo-forming clouds are likely rare due to the high supersaturation of water that is required but may be more common in northern subtropical regions during northern midsummer.
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Affiliation(s)
| | - D. Toledo
- Instituto Nacional de Técnica AerospacialMadridSpain
| | - V. Apestigue
- Instituto Nacional de Técnica AerospacialMadridSpain
| | - I. Arruego
- Instituto Nacional de Técnica AerospacialMadridSpain
| | | | - P. Patel
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
- Mullard Space Science LaboratoryUniversity College LondonLondonUK
| | - S. Guzewich
- NASA Goddard Space Flight CenterGreenbeltMDUSA
| | | | | | - L. Tamppari
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | - J. Maki
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - A. Brown
- Plancius ResearchSeverna ParkMDUSA
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Golombek M, Williams N, Warner NH, Parker T, Williams MG, Daubar I, Calef F, Grant J, Bailey P, Abarca H, Deen R, Ruoff N, Maki J, McEwen A, Baugh N, Block K, Tamppari L, Call J, Ladewig J, Stoltz A, Weems WA, Mora‐Sotomayor L, Torres J, Johnson M, Kennedy T, Sklyanskiy E. Location and Setting of the Mars InSight Lander, Instruments, and Landing Site. Earth Space Sci 2020; 7:e2020EA001248. [PMID: 33134434 PMCID: PMC7583488 DOI: 10.1029/2020ea001248] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/29/2020] [Revised: 09/09/2020] [Accepted: 09/12/2020] [Indexed: 06/11/2023]
Abstract
Knowing precisely where a spacecraft lands on Mars is important for understanding the regional and local context, setting, and the offset between the inertial and cartographic frames. For the InSight spacecraft, the payload of geophysical and environmental sensors also particularly benefits from knowing exactly where the instruments are located. A ~30 cm/pixel image acquired from orbit after landing clearly resolves the lander and the large circular solar panels. This image was carefully georeferenced to a hierarchically generated and coregistered set of decreasing resolution orthoimages and digital elevation models to the established positive east, planetocentric coordinate system. The lander is located at 4.502384°N, 135.623447°E at an elevation of -2,613.426 m with respect to the geoid in Elysium Planitia. Instrument locations (and the magnetometer orientation) are derived by transforming from Instrument Deployment Arm, spacecraft mechanical, and site frames into the cartographic frame. A viewshed created from 1.5 m above the lander and the high-resolution orbital digital elevation model shows the lander is on a shallow regional slope down to the east that reveals crater rims on the east horizon ~400 m and 2.4 km away. A slope up to the north limits the horizon to about 50 m away where three rocks and an eolian bedform are visible on the rim of a degraded crater rim. Azimuths to rocks and craters identified in both surface panoramas and high-resolution orbital images reveal that north in the site frame and the cartographic frame are the same (within 1°).
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Affiliation(s)
- M. Golombek
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - N. Williams
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - N. H. Warner
- Department of Geological SciencesSUNY GeneseoGeneseoNYUSA
| | - T. Parker
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - M. G. Williams
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - I. Daubar
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
- Department of Earth, Environmental, and Planetary SciencesBrown UniversityProvidenceRIUSA
| | - F. Calef
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Grant
- Smithsonian Institution, National Air and Space MuseumWashingtonDCUSA
| | - P. Bailey
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - H. Abarca
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - R. Deen
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - N. Ruoff
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Maki
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - A. McEwen
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | - N. Baugh
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | - K. Block
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | - L. Tamppari
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Call
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | | | | | - L. Mora‐Sotomayor
- Centro de Astrobiología (CSIC/INTA)Instituto Nacional de Técnica AeroespacialMadridSpain
| | - J. Torres
- Centro de Astrobiología (CSIC/INTA)Instituto Nacional de Técnica AeroespacialMadridSpain
| | | | | | - E. Sklyanskiy
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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Smith PH, Tamppari L, Arvidson RE, Bass D, Blaney D, Boynton W, Carswell A, Catling D, Clark B, Duck T, DeJong E, Fisher D, Goetz W, Gunnlaugsson P, Hecht M, Hipkin V, Hoffman J, Hviid S, Keller H, Kounaves S, Lange CF, Lemmon M, Madsen M, Malin M, Markiewicz W, Marshall J, McKay C, Mellon M, Michelangeli D, Ming D, Morris R, Renno N, Pike WT, Staufer U, Stoker C, Taylor P, Whiteway J, Young S, Zent A. Introduction to special section on the Phoenix Mission: Landing Site Characterization Experiments, Mission Overviews, and Expected Science. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003083] [Citation(s) in RCA: 78] [Impact Index Per Article: 4.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Plemmons DH, Mehta M, Clark BC, Kounaves SP, Peach LL, Renno NO, Tamppari L, Young SMM. Effects of the Phoenix Lander descent thruster plume on the Martian surface. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003059] [Citation(s) in RCA: 15] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Arvidson R, Adams D, Bonfiglio G, Christensen P, Cull S, Golombek M, Guinn J, Guinness E, Heet T, Kirk R, Knudson A, Malin M, Mellon M, McEwen A, Mushkin A, Parker T, Seelos F, Seelos K, Smith P, Spencer D, Stein T, Tamppari L. Mars Exploration Program 2007 Phoenix landing site selection and characteristics. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003021] [Citation(s) in RCA: 51] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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