The first Martian year of cloud activity from Mars Science Laboratory (sol 0–800)

Kloos, Jacob L.; Moores, John E.; Lemmon, M. T.; Kass, D. M.; Francis, Raymond; Juárez, Manuel de la Torre; Zorzano, María Paz; Martín-Torres, F. J.

doi:10.1016/j.asr.2015.12.040

Cited by 21 publications

(40 citation statements)

References 14 publications

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“…With a cellular pattern with a characteristic wavelength of the order of the PBL thickness (2–10 km) and advection speeds of the order of 5–10 m/s, quasiperiodic variations in other meteorological properties with periods of a few hundred seconds might be expected and indeed have been observed in the Viking windspeed and seismometer record (Lorenz et al, 2017). On the other hand, higher‐altitude clouds of CO 2 or H 2 O not infrequently have opacities (measured in camera images from the Curiosity rover—e.g., Kloos et al, 2018) of a few percent and, although typically more prominent in the early morning or late afternoon, can occur at all times of day.…”

Section: Short‐term Solar Flux Variationsmentioning

confidence: 99%

Scientific Observations With the InSight Solar Arrays: Dust, Clouds, and Eclipses on Mars

Lorenz

Lemmon

Maki

et al. 2020

Earth and Space Science

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Records of solar array currents recorded by the InSight lander during its first 200 sols on Mars are presented. In addition to the geometric variation in illumination on seasonal and diurnal timescales, the data are influenced by dust suspended in the atmosphere and deposited on the solar panels. Although no dust devils have been detected by InSight's cameras, brief excursions in solar array currents suggest that at least some of the vortices detected by transient pressure drops are accompanied by dust. A step increase in array output (i.e., a "cleaning event") was observed to be directly associated with the passage of a strong vortex. Some quasiperiodic variations in solar array current are suggestive of dust variations in the planetary boundary layer. Nonzero array outputs before sunrise and after sunset are indicative of scattering in the atmosphere: A notable increase in evening twilight currents is observed associated with noctilucent clouds, likely of water or carbon dioxide ice. Finally, although the observations are intermittent (typically a few hours per sol) and at a modest sample rate (one to two samples per minute), three single-sample light dips are seen associated with Phobos eclipses. These results demonstrate that engineering data from solar arrays provide valuable scientific situational awareness of the Martian environment.

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Section: Short‐term Solar Flux Variationsmentioning

confidence: 99%

Scientific Observations With the InSight Solar Arrays: Dust, Clouds, and Eclipses on Mars

Lorenz

Lemmon

Maki

et al. 2020

Earth and Space Science

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“…Others include REMS UV photodiodes (Smith et al 2016) Navcam (e.g. Kloos et al, 2016;Moore et al, 2016), and Mastcam (Lemmon, 2014).…”

Section: Introductionmentioning

confidence: 99%

Retrieval of water vapor column abundance and aerosol properties from ChemCam passive sky spectroscopy

McConnochie

Smith

Wolff

et al. 2018

Icarus

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We derive water vapor column abundances and aerosol properties from Mars Science Laboratory (MSL) ChemCam passive mode observations of scattered sky light. This paper covers the methodology and initial results for water vapor and also provides preliminary results for aerosols. The data set presented here includes the results of 113 observations spanning from Mars Year 31 L s = 291° (March 30, 2013) to Mars Year 33 L s =127° (March 24, 2016).Each ChemCam passive sky observation acquires spectra at two different elevation angles. We fit these spectra with a discrete-ordinates multiple scattering radiative transfer model, using the correlated-k approximation for gas absorption bands. The retrieval proceeds by first fitting the continuum of the ratio of the two elevation angles to solve for aerosol properties, and then fitting the continuum-removed ratio to solve for gas abundances. The final step of the retrieval makes use of the observed CO 2 absorptions and the known CO 2 abundance to correct the retrieved water vapor abundance for the effects of the vertical distribution of scattering aerosols and to derive an aerosol scale height parameter.Our water vapor results give water vapor column abundance with a precision of +/-0.6 precipitable microns and systematic errors no larger than +/-0.3 precipitable microns, assuming uniform vertical mixing. The ChemCam-retrieved water abundances show, with only a few exceptions, the same seasonal behavior and the same timing of seasonal minima and maxima as the TES, CRISM, and REMS-H data sets that we compare them to. However ChemCam-retrieved water abundances are generally lower than zonal and regional scale from-orbit water vapor data, while at the same time being significantly larger than pre-dawn REMS-H abundances. Pending further analysis of REMS-H volume mixing ratio uncertainties, the differences between ChemCam and REMS-H pre-dawn mixing ratios appear to be much too large to be explained by large scale circulations and thus they tend to support the hypothesis of substantial diurnal interactions of water vapor with the surface. Our preliminary aerosol results, meanwhile, show the expected seasonal pattern in dust particle size but also indicate a surprising inter-annual increase in water-ice cloud opacities. Highlights:• We measure water vapor abundances and aerosol properties at Gale Crater, Mars.• Precipitable water column is measured with a precision of +/-0.6 µm.• Measured quantities include dust & ice fractions, particle sizes, and scale heights.• Results suggest substantial diurnal interactions of water vapor with the surface.• A large interannual change in water ice cloud / haze opacity is observed.

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“…While the primary focus of the mission is to investigate the past environment of Mars, it has also conducted numerous studies into the present day environment (Audouard et al, ; Moore et al, ; Pla‐García & Rafkin, ). Among the environmental investigations conducted by Curiosity are studies into the regional cloud activity (Kloos et al, ; Moores, Lemmon, Rafkin, et al, ). From the onset of the mission, Curiosity has executed two separate cloud imaging observations that have captured tenuous, suboptical water ice and dust clouds in the skies of its landing site.…”

Section: Introductionmentioning

confidence: 99%

“…This opacity level was found to be consistent with water ice opacity retrievals from Mars Reconnaissance Orbiter (MRO) Mars Climate Sounder (MCS) collected within 5° of latitude and longitude of Gale Crater, which detected thin clouds ( τ vis =0.03–0.08) between 20 and 50 km in altitude (Moores, Lemmon, Rafkin, et al, ). Kloos et al () extended the results of the ZMs and SHMs to report on observations occurring up to sol 800 ( L S =227° of MY 32), encompassing 1.2 Martian years of observations. With the extension of the data set to beyond a full Martian year, a prominent seasonal trend was observed, as cloud formation was reportedly confined to occur between L S =3°–170° of MY 32.…”

Section: Introductionmentioning

confidence: 99%

Interannual and Diurnal Variability in Water Ice Clouds Observed from MSL Over Two Martian Years

et al. 2018

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We update the results of cloud imaging sequences from the Mars Science Laboratory (MSL) rover Curiosity to complete two Mars years of observations (LS=160° of Mars year (MY) 31 to LS=160° of MY 33). Relatively good seasonal coverage is achieved within the study period, with just over 500 observations obtained, averaging one observation every 2–3 sols. Cloud opacity measurements are made using differential photometry and a simplified radiative transfer method. These opacity measurements are used to assess the interannual variability of the aphelion cloud belt (ACB) for MY 32 and 33. Upon accounting for a statistical bias in the data set, the variation is found to be <30% within uncertainty. Diurnal variation of the ACB is also able to be examined in MY 33 owing to an increased number of early morning observations in this year. Although a gap in data around local noon prevents a complete assessment, we find that cloud opacity is moderately increased in the morning hours (07:00–09:00) compared to the late afternoon (15:00–17:00).

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The first Martian year of cloud activity from Mars Science Laboratory (sol 0–800)

Cited by 21 publications

References 14 publications

Scientific Observations With the InSight Solar Arrays: Dust, Clouds, and Eclipses on Mars

Scientific Observations With the InSight Solar Arrays: Dust, Clouds, and Eclipses on Mars

Retrieval of water vapor column abundance and aerosol properties from ChemCam passive sky spectroscopy

Interannual and Diurnal Variability in Water Ice Clouds Observed from MSL Over Two Martian Years

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