Planetary Waves Traveling Between Mars Science Laboratory and Mars 2020

Battalio, J. Michael; Martínez, G.; Newman, Claire; Juárez, Manuel de la Torre; Sánchez‐Lavega, Agustín; Viúdez‐Moreiras, Daniel

doi:10.1029/2022gl100866

Cited by 10 publications

(9 citation statements)

References 74 publications

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“…Note that thermal oscillations in MEDA and MCD have similar amplitudes (1 K) to those identified by Battalio et al. (2022).…”

Section: Temporal Variations Of Atmospheric and Surface Temperaturessupporting

confidence: 80%

“…The MCD time series is qualitatively similar, although it is based on a statistical description of Mars GCM simulations reconstructing typical variations for Jezero at that seasonal period. Note that thermal oscillations in MEDA and MCD have similar amplitudes (1 K) to those identified by Battalio et al (2022). To assess the influence of the surface thermal inertia, Figure 10b displays the thermal oscillations over a portion of the complete time series.…”

Section: Long-period Waves (Period >1 Sol)mentioning

confidence: 74%

“…Oscillations in atmospheric variables on timescales larger than a sol are generally related to planetary scale waves or the passage of weather fronts. Battalio et al (2022) examined planetary waves from multiple meteorological variables measured by Perseverance and MSL, including temperatures, and compared their results with the Ensemble Mars Atmospheric Reanalysis System (EMARS) data set. According to this work, traveling waves of baroclinic nature with periods of ∼3 sols are found in the temperature data from Perseverance, MSL, and EMARS, being further supported by their analysis in pressure, whereas waves with periods above 8 sols are attributed to barotropic instabilities and possible weather fronts.…”

Section: Long-period Waves (Period >1 Sol)mentioning

confidence: 99%

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Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements

et al. 2023

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The Mars Environmental Dynamics Analyzer instrument on Mars 2020 has five Atmospheric Temperature Sensors at two altitudes (0.84 and 1.45 m) plus a Thermal InfraRed Sensor that measures temperatures on the surface and at ∼40 m. We analyze the measurements from these sensors to describe the evolution of temperatures in Jezero up to mission sol 400 (solar longitude LS = 13°–203°). The diurnal thermal cycle is characterized by a daytime convective period and a nocturnal stable atmosphere with a variable thermal inversion. We find a linear relationship between the daytime temperature fluctuations and the vertical thermal gradient with temperature fluctuations that peak at noon with typical values of 2.5 K at 1.45 m. In the late afternoon (∼17:00 Local True Solar Time), the atmosphere becomes vertically isothermal with vanishing fluctuations. We observe very small seasonal changes in air temperatures during the period analyzed. This is related to small changes in solar irradiation and dust opacity. However, we find significant changes in surface temperatures that are related to the variety of thermal inertias of the terrains explored along the traverse of Perseverance. These changes strongly influence the vertical thermal gradient, breaking the nighttime thermal inversion over terrains of high thermal inertia. We explore possible detections of atmospheric tides on near‐surface temperatures and we examine variations in temperatures over timescales of a few sols that could be indicative of atmospheric waves affecting near‐surface temperatures. We also discuss temperatures during a regional dust storm at LS = 153°–156° that simultaneously warmed the near surface atmosphere while cooling the surface.

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“…Note that thermal oscillations in MEDA and MCD have similar amplitudes (1 K) to those identified by Battalio et al. (2022).…”

Section: Temporal Variations Of Atmospheric and Surface Temperaturessupporting

confidence: 80%

Section: Long-period Waves (Period >1 Sol)mentioning

confidence: 74%

Section: Long-period Waves (Period >1 Sol)mentioning

confidence: 99%

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Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements

et al. 2023

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“…As suggested by previous studies, the dynamic response can be related to atmospheric waves (such as PWs and GWs) (Battalio et al, 2022;Kuroda et al, 2020;Shaposhnikov et al, 2022), which can transport momentum by interact with the mean flow, affecting the residual circulation and the temperature (Andrews et al, 1987). As shown in Eq.…”

Section: Resultsmentioning

confidence: 95%

The Atmospheric Response to an Unusual Early-Year Martian Dust Storm

Sun,

Yang,

Fang

et al. 2024

Preprint

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During the northern spring (approximately Ls≈33°) in Martian Year 35, Mars experienced an unusual dust storm characterized by significantly increased dust in the northern troposphere. As observed by the Mars Climate Sounder (MCS), temperature significantly increases in the mid-latitude troposphere of both hemispheres and decreases in the northern mesosphere during the event. The temperature response simulated by the Martian General Circulation Model (GCM) agrees with the MCS observations. The radiative heating from dust is responsible for the increased temperature in the northern troposphere. In contrast, the dynamic heating/cooling contributes to the temperature variations in the southern troposphere and northern mesosphere. The increased dissipation of planetary waves enhances the residual meridional circulation and causes the temperature warming in the Southern Hemisphere. In addition, the enhanced meridional circulation related to this event leads to ~36% increase in water vapor transport from the Northern to the Southern Hemisphere as compared to the net interhemispheric transport over an entire Martian Year.

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“…In addition to the mean circulation, thermal tides and planetary waves can arise from perturbations in the atmosphere (such as from the differential heating of the surface by solar radiation) and manifest as oscillations in atmospheric temperature, pressure, and density (Forbes et al 2002) with periods ranging from less than a sol to several sols. These phenomena and their effects on the local circulation at Gale crater have been well documented (e.g., Haberle et al 2014;Guzewich et al 2016;Martínez et al 2017;Viúdez-Moreiras et al 2020a;Battalio et al 2022). Similar to transport and mixing processes, tides and waves do not change the total amount of noncondensible species in the atmosphere.…”

Section: Msl Sam O 2 Vmr Observationsmentioning

confidence: 94%

Evaluating Atmospheric and Surface Drivers for O₂ Variations at Gale Crater as Observed by MSL SAM

Lo,

Atreya,

Wong

et al. 2024

Planet. Sci. J.

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We explore and evaluate various processes that could drive the variations in the volume mixing ratio (VMR) of atmospheric O2 observed by the quadrupole mass spectrometer (QMS) of the Sample Analysis at Mars (SAM) instrument suite on the Mars Science Laboratory (MSL) Curiosity rover. First reported by Trainer et al. (2019), these ∼20% variations in the O2 VMR on a seasonal timescale over Mars Years 31–34, in excess of circulation and transport effects driven by the seasonal condensation and sublimation of CO2 at the poles, are significantly shorter than the modeled O2 photochemical lifetime. While there remains significant uncertainty about the various processes we investigated (atmospheric photochemistry, surface oxychlorines and H2O2, dissolution from brines, and airborne dust), the most plausible driver is surface oxychlorines, exchanging O2 with the atmosphere through decomposition by solar ultraviolet and regeneration via O3. A decrease in O3 from increased atmospheric H2O would reduce the removal rate of O2 from the atmosphere to form oxychlorines at the surface. This is consistent with the tentative observation that increases in O2 are associated with increases in water vapor. A lack of correlation with the local surface geology along Curiosity’s traverse within Gale crater, the nonuniqueness of the relevant processes to Gale crater, and the short mixing timescales of the atmosphere all suggest that the O2 variations are a regional, or even global, phenomenon. Nonetheless, further laboratory experiments and modeling are required to accurately scale the laboratory-measured rates to Martian conditions and to fully elucidate the driving mechanisms.

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Planetary Waves Traveling Between Mars Science Laboratory and Mars 2020

Cited by 10 publications

References 74 publications

Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements

Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements

The Atmospheric Response to an Unusual Early-Year Martian Dust Storm

Evaluating Atmospheric and Surface Drivers for O₂ Variations at Gale Crater as Observed by MSL SAM

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Planetary Waves Traveling Between Mars Science Laboratory and Mars 2020

Cited by 10 publications

References 74 publications

Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements

Near Surface Atmospheric Temperatures at Jezero From Mars 2020 MEDA Measurements

The Atmospheric Response to an Unusual Early-Year Martian Dust Storm

Evaluating Atmospheric and Surface Drivers for O2 Variations at Gale Crater as Observed by MSL SAM

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Product

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Evaluating Atmospheric and Surface Drivers for O₂ Variations at Gale Crater as Observed by MSL SAM