Winds at the Mars 2020 Landing Site. 2. Wind Variability and Turbulence

Viúdez‐Moreiras, Daniel; Juárez, Manuel de la Torre; Apéstigue, Víctor; Lorenz, Ralph D.; Apéstigue, V.; Guzewich, Scott D.; Newman, Claire; Sullivan, Robert; Hueso, R.; Toledo, Daniel; Lemmon, M. T.; Smith, M. D.; Newman, C. E.; Sánchez‐Lavega, Agustín; Rodríguez‐Manfredi, J. A.; Richardson, M. I.; Harri, A. M.; Tamppari, L. K.; Arruego, Ignacio; Bell, James F.

doi:10.1029/2022je007523

Cited by 13 publications

(11 citation statements)

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“…The InSight pressure data demonstrated a shallower slope that expected for the inertial regime (Banfield et al, 2020;Temel et al, 2022). For Perseverance at Jezero, Viúdez-Moreiras, Torre, et al (2022) 2022) showed steeper slopes (−2.6 and −1.9 between 0.1 and 1 Hz) for temperature. Of particular note, on Mars the dissipative regime begins at lower frequencies than on Earth.…”

Section: The Martian Planetary Boundary Layermentioning

confidence: 80%

“…The Perseverance wind speeds were collected on a 1 hr on 1 hr off cadence and can be up to 2 Hz. Viúdez-Moreiras, Lemmon, et al (2022);Viúdez-Moreiras, Torre, et al (2022) have demonstrated that the winds at Jezero are generally calmer than other landing sites but have a slightly higher turbulent intensity than at InSight. However, several boards of the Perseverance wind sensor were damaged (Lemmon et al, 2022;Viúdez-Moreiras, Lemmon, et al, 2022) due to wind-induced sand particle impacts especially during a regional dust storm on sols 313 and 315 (Hueso et al, 2022b), thus hindering the wind retrieval with the same accuracy.…”

Section: The Martian Planetary Boundary Layermentioning

confidence: 98%

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Wind and Turbulence Observations With the Mars Microphone on Perseverance

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We utilize SuperCam's Mars microphone to provide information on wind speed and turbulence at high frequencies on Mars. To do so, we first demonstrate the sensitivity of the microphone signal level to wind speed, yielding a power law dependence. We then show the relationship between the microphone signal level and pressure, air and ground temperatures. A calibration function is constructed using Gaussian process regression (a machine learning technique) taking the microphone signal and air temperature as inputs to produce an estimate of the wind speed. This provides a high rate wind speed estimate on Mars, with a sample every 0.01 s. As a result, we determine the fast fluctuations of the wind at Jezero crater which highlights the nature of wind gusts over the Martian day. To analyze the turbulent behavior of this wind speed estimate, we calculate its normalized standard deviation, known as gustiness. To characterize the behavior of this high frequency turbulent intensity at Jezero crater, correlations are shown between the evaluated gustiness statistic and pressure drop rates/sizes, temperature and energy fluxes. This has implications for future atmospheric models on Mars, taking into account turbulence at the finest scales.

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Section: The Martian Planetary Boundary Layermentioning

confidence: 80%

Section: The Martian Planetary Boundary Layermentioning

confidence: 98%

Wind and Turbulence Observations With the Mars Microphone on Perseverance

et al. 2023

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“…A close encounter with a dust devil (DD) on sol 313 at 13:42 hr local true solar time (LTST) further damaged WS2 (see the companion paper, Viúdez‐Moreiras et al. (2022), hereafter referred to as part 2). Two sols later (sol 315 at 14:24 hr LTST), the damage was produced on WS1 and the MEDA WS was unavailable to provide wind data, leaving only three operative sensor boards: one on WS2 and two on WS1.…”

Section: Methods: the Mars 2020 Meda Wind Sensor And Observationsmentioning

confidence: 99%

Winds at the Mars 2020 Landing Site: 1. Near‐Surface Wind Patterns at Jezero Crater

et al. 2022

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IntroductionNASA's Mars 2020 Perseverance rover successfully landed close to the western rim of Jezero crater (18.44°N, 77.45°E) on 18 February 2021 (areocentric solar longitude, L s ∼ 5°). The rover is seeking signs of potential ancient life on Mars and preparing, for the first time, a set of samples for possible return to Earth (Farley et al., 2020). Among the mission objectives, Mars 2020 should enable future Mars exploration focused on manned missions with a characterization of the atmospheric environment. To fulfill this requirement, the Mars Environmental

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“…Data from both booms are combined to produce horizontal wind speed and direction values of the highest confidence, with accuracies of ±1 m/s and a resolution of 0.5 m/s for wind speeds <10 m/s, and 10% of the measurement and 0.1 m/s for wind speeds between 10 and 40 m/s. The WS was damaged by a dust devil during the regional dust storm around sols 312–318 (Ls 152°–156°) (Hueso et al., 2022; Lemmon et al., 2022; Viúdez‐Moreiras, de la Torre, et al., 2022; Viúdez‐Moreiras, Lemmon, et al., 2022). Thus, WS measurements of the highest confidence are only available for the first 313 sols of the mission (Figure S1 in Supporting Information ).…”

Section: The Meda Instrumentmentioning

confidence: 99%

Surface Energy Budget, Albedo, and Thermal Inertia at Jezero Crater, Mars, as Observed From the Mars 2020 MEDA Instrument

et al. 2023

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The Mars Environmental Dynamics Analyzer (MEDA) on board Perseverance includes first-of-its-kind sensors measuring the incident and reflected solar flux, the downwelling atmospheric IR flux, and the upwelling IR flux emitted by the surface. We use these measurements for the first 350 sols of the Mars 2020 mission (L s ∼ 6°-174° in Martian Year 36) to determine the surface radiative budget on Mars and to calculate the broadband albedo (0.3-3 μm) as a function of the illumination and viewing geometry. Together with MEDA measurements of ground temperature, we calculate the thermal inertia for homogeneous terrains without the need for numerical thermal models. We found that (a) the observed downwelling atmospheric IR flux is significantly lower than the model predictions. This is likely caused by the strong diurnal variation in aerosol opacity measured by MEDA, which is not accounted for by numerical models. (b) The albedo presents a marked non-Lambertian behavior, with lowest values near noon and highest values corresponding to low phase angles (i.e., Sun behind the observer). (c) Thermal inertia values ranged between 180 (sand dune) and 605 (bedrock-dominated material) SI units. (d) Averages of albedo and thermal inertia (spatial resolution of ∼3-4 m 2 ) along Perseverance's traverse are in very good agreement with collocated retrievals of thermal inertia from Thermal Emission Imaging System (spatial resolution of 100 m per pixel) and of bolometric albedo in the 0.25-2.9 μm range from (spatial resolution of ∼300 km 2 ). The results presented here are important to validate model predictions and provide ground-truth to orbital measurements. Plain Language SummaryWe analyzed first-of-its-kind measurements from the weather station on board NASA's Perseverance rover. These include the incident solar radiation and the amount that is reflected by the surface, as well as the thermal atmospheric forcing (greenhouse effect) and the thermal heat released by the surface. These measurements comprise the radiant energy budget, which is fundamental to understanding Mars' weather through its impact on temperatures. From the solar measurements, we obtained the surface reflectance for a variety of illuminating and viewing geometries. We found that the thermal atmospheric forcing is weaker than expected from models, likely because of the strong diurnal variation in atmospheric aerosols observed by the rover, which is not accounted for by models. We also found that the surface reflectance is not uniform from all directions, but that it decreases when the Sun is highest in the sky (near noon) and increases when the Sun is directly behind the observer (sunset and sunrise), and thus the shadows cast by their roughness elements (e.g., pores and pits) are minimized. Because models neither consider diurnal variations in atmospheric aerosols nor in the surface reflectance, the results presented here are important to validate model predictions for future human exploration. MARTÍNEZ ET AL.

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Winds at the Mars 2020 Landing Site. 2. Wind Variability and Turbulence

Cited by 13 publications

References 59 publications

Wind and Turbulence Observations With the Mars Microphone on Perseverance

Wind and Turbulence Observations With the Mars Microphone on Perseverance

Winds at the Mars 2020 Landing Site: 1. Near‐Surface Wind Patterns at Jezero Crater

Surface Energy Budget, Albedo, and Thermal Inertia at Jezero Crater, Mars, as Observed From the Mars 2020 MEDA Instrument

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