Observational evidence of a suppressed planetary boundary layer in northern Gale Crater, Mars as seen by the Navcam instrument onboard the Mars Science Laboratory rover

Moores, John E.; Lemmon, M. T.; Kahanpää, Henrik; Rafkin, Scot; Francis, Raymond; Pla‐García, Jorge; Bean, Keri; Haberle, R. M.; Newman, C. E.; Mischna, M. A.; Vasavada, A. R.; Juárez, Manuel de la Torre; Rennó, N. O.; Bell, James F.; Calef, F.; Cantor, B. A.; McConnochie, T. H.; Harri, A. M.; Genzer, M.; Wong, Michael H.; Smith, M. D.; Martín-Torres, F. J.; Zorzano, María Paz; Kemppinen, Osku; McCullough, Emily

doi:10.1016/j.icarus.2014.09.020

Cited by 69 publications

(106 citation statements)

References 34 publications

(49 reference statements)

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“…This limit is roughly in agreement with the threshold of ∆p t = 2.0 Pa obtained by Moores et al (2015), which was based on comparing the statistics of vortex detections in the image and pressure data measured by Pathfinder. [Spiga et al, 2016] for more details on LES).…”

supporting

confidence: 88%

“…Pathfinder (Murphy and Nelli 2002;Ferri et al 2003), Phoenix (Ellehoj et al 2010) and MSL Curiosity (Moores et al 2015;Kahanpää et al 2016;Steakley and Murphy 2016). Pathfinder and Phoenix operated for only a few months and took a small number of images suitable for a dust devil survey.…”

mentioning

confidence: 99%

“…Thus only 14 and 37 dust devils were identified from the images taken by these landers, respectively (Ferri et al 2003;Ellehoj et al 2010). Curiosity has operated to date for more than one martian year, but landed on an area where the dust devil activity is low and was thus able to detect only one plausible dust devil during its first Earth year on Mars (first 360 sols), despite an intensive imaging campaign of "dust devil search movies" (Moores et al 2015). No more dust devils have been detected between sols 361 and 681 (J.…”

mentioning

confidence: 99%

“…A distinctive feature of these pressure drops is that they are small: less than 4.8 Pa, 3.6 Pa, and 3.0 Pa for Pathfinder, Phoenix, and Curiosity (first 681 sols), respectively (Murphy and Nelli 2002;Ellehoj et al 2010;Kahanpää et al 2016;Steakley and Murphy 2016). Moores et al (2015) compared the statistics of dust devil detections in the image data and pressure data of Pathfinder. A prediction of the number of dust devils that should be visible in the images was calculated based on the assumption that all identified pressure drops with magnitude greater than a preset threshold, ∆p t , were caused by dust-lifting vortices.…”

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confidence: 99%

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Dust Devil Sediment Transport: From Lab to Field to Global Impact

et al. 2016

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The impact of dust aerosols on the climate and environment of Earth and Mars is complex and forms a major area of research. A difficulty arises in estimating the contribution of small-scale dust devils to the total dust aerosol. This difficulty is due to uncertainties in the amount of dust lifted by individual dust devils, the frequency of dust devil occurrence, and the lack of statistical generality of individual experiments and observations. In this paper, we review results of observational, laboratory, and modeling studies and provide an overview of dust devil dust transport on various spatio-temporal scales as obtained with the different research approaches. Methods used for the investigation of dust devils on Earth and Mars vary. For example, while the use of imagery for the investigation of dust devil occurrence frequency is common practice for Mars, this is less so the case for Earth. Modeling approaches for Earth and Mars are similar in that they are based on the same underlying

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confidence: 88%

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confidence: 99%

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confidence: 99%

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confidence: 99%

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Dust Devil Sediment Transport: From Lab to Field to Global Impact

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“…On Mars, cameras and meteorological in situ/remote sensing instrumentation on landers/orbiters have substantially advanced knowledge about Martian dust devils, thereby inspiring further research (e.g. Ryan and Lucich 1983;Thomas and Gierasch 1985;Schofield et al 1997;Cantor et al 2006;Greeley et al 2010;Ellehoj et al 2010;Moores et al 2015). In addition, laboratory experiments and numerical modeling are powerful techniques to investigate dust devils (e.g.…”

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confidence: 99%

Dust Devil Sediment Transport: From Lab to Field to Global Impact

Klose¹,

Jemmett-Smith²,

Kahanpää³

et al. 2017

Space Sciences Series of ISSI

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Dust deposition on the decks of the Mars Exploration Rovers: 10 years of dust dynamics on the Panoramic Camera calibration targets

Kinch

Bell

Goetz

et al. 2015

Earth and Space Science

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The Panoramic Cameras on NASA's Mars Exploration Rovers have each returned more than 17,000 images of their calibration targets. In order to make optimal use of this data set for reflectance calibration, a correction must be made for the presence of air fall dust. Here we present an improved dust correction procedure based on a two‐layer scattering model, and we present a dust reflectance spectrum derived from long‐term trends in the data set. The dust on the calibration targets appears brighter than dusty areas of the Martian surface. We derive detailed histories of dust deposition and removal revealing two distinct environments: At the Spirit landing site, half the year is dominated by dust deposition, the other half by dust removal, usually in brief, sharp events. At the Opportunity landing site the Martian year has a semiannual dust cycle with dust removal happening gradually throughout two removal seasons each year. The highest observed optical depth of settled dust on the calibration target is 1.5 on Spirit and 1.1 on Opportunity (at 601 nm). We derive a general prediction for dust deposition rates of 0.004 ± 0.001 in units of surface optical depth deposited per sol (Martian solar day) per unit atmospheric optical depth. We expect this procedure to lead to improved reflectance‐calibration of the Panoramic Camera data set. In addition, it is easily adapted to similar data sets from other missions in order to deliver improved reflectance calibration as well as data on dust reflectance properties and deposition and removal history.

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Observational evidence of a suppressed planetary boundary layer in northern Gale Crater, Mars as seen by the Navcam instrument onboard the Mars Science Laboratory rover

Cited by 69 publications

References 34 publications

Dust Devil Sediment Transport: From Lab to Field to Global Impact

Dust Devil Sediment Transport: From Lab to Field to Global Impact

Dust Devil Sediment Transport: From Lab to Field to Global Impact

Dust deposition on the decks of the Mars Exploration Rovers: 10 years of dust dynamics on the Panoramic Camera calibration targets

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