Curiosity observations and column model integrations for a martian global dust event

Savijärvi, Hannu; Martínez, G.; Harri, A. M.; Paton, Mark

doi:10.1016/j.icarus.2019.113515

Cited by 14 publications

(19 citation statements)

References 24 publications

(23 reference statements)

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“…When θ < 55° (corresponding to about 60% of UV measurements performed with the Sun above the horizon, and covering the 8–15 LMST period at L s ∼ 100°–250° and the 9–16 LMST period during the rest of the year), we converted hourly values of corrected UV fluxes in the 200–380 nm to broadband (200–3000 nm) shortwave fluxes using the radiative transfer model COMIMART (Vicente‐Retortillo et al., 2015). Dust radiative properties involved in the calculations were derived from CRISM (Wolff et al., 2009), MARCI (Wolff et al., 2010), Mastcam, and REMS (Savijärvi et al., 2020) observations. These properties depend on wavelength (Wolff et al., 2009), with the single scattering albedo in the UV range being smaller than the mean value in the entire shortwave range.…”

Section: Methodsmentioning

confidence: 99%

“…The diurnal variation in LW↓ is shown in Figure 9 and presents two local maxima, with a first peak in the 7–10 LMST period and a second in the 15–19 LMST period. This behavior is completely unexpected, as numerical models such as the SCM and THM or the Mars Climate Database (MCD) (Forget et al., 1999; Madeleine et al., 2011) built using the LMD Martian Atmospheric General Circulation Model predict only the 15–19 LMST peak following dust emission from the Sun‐heated late afternoon air column (e.g., Savijärvi et al., 2020). While the 7–10 LMST peak in LW↓ may be due to its large relative error (∼20%–100% depending on Ls; Figure 6d), the two maxima exist for the vast majority of the sols, regardless of the season, environmental conditions, and types of terrains traversed by the Curiosity rover.…”

Section: Interannual Seasonal and Diurnal Variation Of The Sebmentioning

confidence: 99%

“…3 of 25 environmental outputs (e.g., temperature and radiation fluxes) strongly depend on the simulated SEB values (Greybush et al, 2019;Newman et al, 2019;Pla-Garcia et al, 2016;Savijärvi et al, 2020;Spiga et al, 2020).…”

mentioning

confidence: 99%

“…In combination with numerical models, the determination of the downwelling SW and LW radiative fluxes provides an excellent opportunity to determine aerosol abundances and their variations (Smith et al, 2016;Vicente-Retortillo et al, 2021) to validate aerosol radiative properties for a range of dust conditions, including global dust storms (Savijärvi et al, 2020), and to indirectly detect the presence of water ice clouds at nighttime (de la Torre-Juarez et al, 2019;Vasavada et al, 2017). Furthermore, the determination of the downwelling SW radiative and turbulent heat fluxes is important to understand the energy available for solar-powered missions and to infer the periodic removal of dust from solar panels caused by convective phenomena such as dust devils (Lorenz et al, 2020;Vicente-Retortillo et al, 2018).…”

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confidence: 99%

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The Surface Energy Budget at Gale Crater During the First 2500 Sols of the Mars Science Laboratory Mission

et al. 2021

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We use in situ environmental measurements by the Mars Science Laboratory (MSL) mission to obtain the surface energy budget (SEB) across Curiosity's traverse during the first 2500 sols of the mission. This includes values of the downwelling shortwave solar radiation, the upwelling solar radiation reflected by the surface, the downwelling longwave radiation from the atmosphere, the upwelling longwave radiation emitted by the surface, the sensible heat flux associated with turbulent motions, and the latent heat flux associated with water phase changes. We then analyze their temporal variation on different timescales and relate this to the mechanisms causing these variations. Through its Rover Environmental Monitoring Station, MSL allows for a more accurate determination of the SEB than its predecessors on Mars. Moreover, the unprecedented duration, cadence, and frequency of MSL environmental observations allow for analyses of the SEB from diurnal to interannual timescales. The results presented in this article can be used to evaluate the consistency with predictions from atmospheric numerical models, to validate aerosol radiative properties under a range of dust conditions, to understand the energy available for solar-powered missions, and to enable comparisons with measurements of the SEB by the Perseverance rover at Jezero crater.Plain Language Summary The primary energy input at the Martian surface is the solar radiation, which depends on the time of the day and season, geographical location (latitude and altitude), and atmospheric dust and gas abundances. Another energy input is the thermal atmospheric forcing, which depends on the vertical distribution of dust and water ice aerosols as well as CO 2 and H 2 O molecules. Together with the reflected solar radiation and the thermal radiation emitted by the surface, these four terms make up the net radiative forcing of the surface. In response to it, energy outputs as turbulent motions and water phase changes emerge to cool down/warm up the ground. The remaining energy is available to control the thermal environment in the surface and shallow subsurface through conduction into the soil. By using first-of-their-kind measurements from the Mars Science Laboratory mission, we calculate the energy inputs and outputs across Curiosity's traverse over the first 2500 Martian days of the mission. We then analyze their temporal variations and relate this to the mechanisms causing such variations. An accurate determination of the surface energy budget is key to preparing for the human exploration of Mars because it contributes to improvements in the predictive capabilities of numerical models.MARTÍNEZ ET AL.

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Section: Methodsmentioning

confidence: 99%

Section: Interannual Seasonal and Diurnal Variation Of The Sebmentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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The Surface Energy Budget at Gale Crater During the First 2500 Sols of the Mars Science Laboratory Mission

et al. 2021

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“…It was hypothesized in Viúdez-Moreiras et al (2019) that the combined effect of a reduction in the strength of an adsorption and desorption mechanism in the regolith, which is likely driving the diurnal cycle in the near-surface water vapor abundance, and the enhanced vertical mixing suggested at night during the dust storm period could be driving the observed effect in the diurnal cycle considering that the inferred water vapor abundances during the GDS are correct. Savijärvi et al (2020) attempted to simulate the MY34 GDS surface water abundance within Gale crater by means of a one-dimensional model and further assumptions, but simulations did not match the observations, and they proposed an additional source of water vapor to minimize the model mismatch. Additional and accurate surface measurements will contribute to discern the role of exchange with the regolith.…”

Section: Introductionmentioning

confidence: 99%

Effects of a Large Dust Storm in the Near‐Surface Atmosphere as Measured by InSight in Elysium Planitia, Mars. Comparison With Contemporaneous Measurements by Mars Science Laboratory

et al. 2020

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NASA's InSight landed in Elysium Planitia (~4.5°N,136°E) at Ls ~ 296° (November 2018), right after the decay of the 2018 Global Dust Storm (GDS) and before the onset of the 2019 Large Dust Storm (LDS) at Ls ~ 320° (January 2019). InSight's cameras observed a rise in the atmospheric opacities during the storm from ~0.7 to ~1.9, similarly to contemporaneous measurements by Curiosity in Gale crater. Pressure tides were strongly affected at the locations of InSight and Curiosity. In particular, the diurnal pressure mode experienced an abrupt increase during the onset of the LDS, similar to that measured by Curiosity, most likely due to longitudinally asymmetric dust loading. Later, the dust was redistributed around the planet and the semidiurnal mode evolved according to dust opacity in both missions. Before and after the onset of the storm, the observed wind patterns resulted from the interaction between regional and local slope flows induced by topography, which all produced a diurnal perturbation superimposed on a mean flow, dominated by the Hadley cell but with modifications due to channeling effects from the regional topography. However, the onset of the LDS modified this to a scenario consistent with enhanced tidal flows. The local air temperatures are strongly perturbed by the lander's thermal effects, and their retrieval significantly depends on wind patterns, which changed during the course of the dust storm. Observations suggest a decrease in convective vortices during the dust storm; however, vortex activity remained strong during the storm's onset due to the increase in wind speeds.

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The Mars Environmental Dynamics Analyzer, MEDA. A Suite of Environmental Sensors for the Mars 2020 Mission

et al. 2021

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NASA’s Mars 2020 (M2020) rover mission includes a suite of sensors to monitor current environmental conditions near the surface of Mars and to constrain bulk aerosol properties from changes in atmospheric radiation at the surface. The Mars Environmental Dynamics Analyzer (MEDA) consists of a set of meteorological sensors including wind sensor, a barometer, a relative humidity sensor, a set of 5 thermocouples to measure atmospheric temperature at ∼1.5 m and ∼0.5 m above the surface, a set of thermopiles to characterize the thermal IR brightness temperatures of the surface and the lower atmosphere. MEDA adds a radiation and dust sensor to monitor the optical atmospheric properties that can be used to infer bulk aerosol physical properties such as particle size distribution, non-sphericity, and concentration. The MEDA package and its scientific purpose are described in this document as well as how it responded to the calibration tests and how it helps prepare for the human exploration of Mars. A comparison is also presented to previous environmental monitoring payloads landed on Mars on the Viking, Pathfinder, Phoenix, MSL, and InSight spacecraft.

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Curiosity observations and column model integrations for a martian global dust event

Cited by 14 publications

References 24 publications

The Surface Energy Budget at Gale Crater During the First 2500 Sols of the Mars Science Laboratory Mission

The Surface Energy Budget at Gale Crater During the First 2500 Sols of the Mars Science Laboratory Mission

Effects of a Large Dust Storm in the Near‐Surface Atmosphere as Measured by InSight in Elysium Planitia, Mars. Comparison With Contemporaneous Measurements by Mars Science Laboratory

The Mars Environmental Dynamics Analyzer, MEDA. A Suite of Environmental Sensors for the Mars 2020 Mission

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