Observations of Ubiquitous Nighttime Temperature Inversions in Mars' Tropics After Large‐Scale Dust Storms

Steele, Liam; Kleinboehl, A.; Kass, D. M.

doi:10.1029/2021gl092651

Cited by 8 publications

(10 citation statements)

References 33 publications

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“…The B‐storm period did not produce a measurable opacity signature in Gale during the years considered. This is consistent with the observation (Steele et al., 2021) that it has a weak influence on equatorial and southern latitudes. The zonally averaged CDOD shows it as a continuation of the A‐storm period where minor storms in the southernmost latitudes add some dust.…”

Section: Resultssupporting

confidence: 94%

“…Four periods may be identified based on the timing of the onset and growth phases of regional storms. Given the different period definitions available in the literature, and the Gale‐based analysis presented here, we use a definition based on the inflection points from the start of Mars Science Laboratory Mastcam (MSL MCAM) opacity growth at Gale to shortly after its peak over the years covered here: the pre‐equinox, Z period from L s ∼ 120°–160° (M. Battalio & Wang, 2019; Steele et al., 2021; Wang & Richardson, 2015), the post‐equinox, “A” period, from L s ∼ 190°–240°, the near‐solstice, “B” period, from L s ∼ 245°–295°, and the post‐solstice, “C” period, from L s ∼ 300°–335° (Kass et al., 2016). While A‐ and C‐period storms have their origin in the northern polar latitudes, some are able to flush south to the equator or into the southern hemisphere through longitudinal corridors to the east of major topography and thus can affect the whole planet.…”

Section: Introductionmentioning

confidence: 99%

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Mars Surface Pressure Oscillations as Precursors of Large Dust Storms Reaching Gale

et al. 2022

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Modeling and observations have long demonstrated that Martian dust storms strongly interfere with global circulation patterns and change the diurnal and semidiurnal pressure variability as well as oscillations with periods greater than one sol associated with planetary waves. As of early 2022, five Mars years of pressure data have been collected by the Curiosity Rover in Gale crater with the Rover Environmental Monitoring Station (REMS). A combination of signal filtering techniques is used to search for pressure signatures that might warn large‐scale dust storms reaching Gale. The analysis combines an exploration of changes in both baroclinic waves and thermal tides for the first time to our knowledge. Focusing on the periods preceding local opacity increases as detected by Curiosity's Mastcam observations, the pressure analysis shows changes in the coupling between the diurnal pressure tide and quasi‐diurnal Kelvin wave, as well as in the temporal evolution of baroclinic waves that are harbingers of the larger dust storms. Changes in the phasing between Kelvin waves and diurnal tides are found to be precursors for the growth phase of periods Z (defined here as Ls ∼ 120°–160°), A (Ls ∼ 190°–240°), and C (Ls ∼ 300°–335°) dust storms. Changes in multi‐sol pressure oscillations also help predict the occurrence of A, B (Ls ∼ 245°–295°), and C storms. The specific pressure oscillations preceding each storm period are likely to be signatures of the large‐scale circulation patterns that enable the growth and propagation of the storm fronts.

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Section: Resultssupporting

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Mars Surface Pressure Oscillations as Precursors of Large Dust Storms Reaching Gale

et al. 2022

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“…Note that Steele et al. (2021) also reported nighttime temperature inversions in the wake of major dust storms. The inversions are strongest around higher‐elevation regions, suggesting they form due to a combination of topographically excited tides and cloud radiative cooling.…”

Section: Discussionmentioning

confidence: 96%

“…However, the horizontal distribution of both the Lp‐ and Mp‐layer GWs and the detached tropical dust layer shows less correlation with the topography during the decay phase than before the dust storm (Figure 8a compared with Figure S4a in Supporting Information ), implying a more complicated generation mechanism during storm time. The peaks in the zonal distribution of both Mp‐layer GWs and the detached dust layer and their agreement suggest that these two phenomena may be caused or related to the same dynamical phenomenon, such as thermal tides induced temperature inversion (Steele et al., 2021). The longitudinal variations in GW activity may also result from the GW‐tidal interaction just like that in the Erath atmosphere (Fritts & Vincent, 1987).…”

Section: Discussionmentioning

confidence: 96%

“…This layer is also prominent in the decay phase after the A or C storm peak, as shown in Figure 5, in good agreement with the evolution of Mp-layer GWs, including the southward tilt with time. Note that Steele et al (2021) also reported nighttime temperature inversions in the wake of major dust storms. The inversions are strongest around higher-elevation regions, suggesting they form due to a combination of topographically excited tides and cloud radiative cooling.…”

Section: Discussionmentioning

confidence: 97%

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Gravity Waves in Different Atmospheric Layers During Martian Dust Storms

et al. 2022

JGR Planets

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Gravity waves (GWs) are relatively small-scale dynamical phenomena that can shape the atmospheric structure and circulation by transporting energy and momentum across distances and atmospheric layers. Though excited mainly in the lower atmosphere, the primary wave influence of GWs occur in the middle and upper atmosphere due to decreasing density and increasing wave amplitudes with altitude. The dynamical effects of GW depend on their wavelength, frequency, and phase speed characteristics, which are mainly determined by their exciting sources, for example, orography, convection, and jet/front systems (Fritts & Alexander, 2003).Martian GWs have been detected using temperature or density profiles by remote sensing or in situ measurements. Rovers and landers such as Curiosity and InSight have detected GW signals near the surface, either excited by topography or convections (Banfield et al., 2020;Guzewich et al., 2021). Lower and middle atmospheric GW activity and their propagation are mainly observed through radio occultation and thermal infrared sounding by orbiters like the Thermal Emission Spectrometer (TES) onboard Mars Global Surveyor (MGS) and the Mars Abstract Gravity waves (GWs) are ubiquitous in the Martian atmosphere and critical for coupling the entire atmospheric system. Recent observations reveal a significant enhancement of thermospheric GW activity in global dust storm conditions, which could increase hydrogen escape. However, the source of these highaltitude GWs and their link to the lower atmosphere are still unknown. We investigate detailed GW distributions and evolutions in three altitude ranges covering the lower, middle, and middle-to-upper transition layers (Lp, Mp, and Hp) of the Martian atmosphere based on multiyear observations from Mars Climate Sounder. The nighttime Mp-layer GWs in the northern tropical region increase significantly after the peak time of regional dust storms, with potential energy 4 times larger than before or at other latitudes. These GWs correlate well with a zonally distributed detached dust layer during storm time, both of which may be generated by a tropical jet system. The upper atmospheric GWs observed during global dust storms are mainly excited in the Hp-layer (∼50-70 km) above the main dust layer, except for Mars year 28 global dust storm, when the polar jet in the Mp-layer (∼30-50 km) at high northern latitudes may be a major excitation source.Plain Language Summary Gravity waves (GWs), a common phenomenon often experienced when encountering airplane turbulence, are important for the movement and structure of the Martian atmosphere. Recent observations found that in very large dust storms spreading over the entire planet, GW activity at an altitude above ∼80 km strongly increases and can promote the process of water escape from Mars. However, the source of these high-altitude GWs and their connection with the lower atmosphere is still unknown. This work studied the detailed GW distribution and evolution throughout the Martian atmosphere from near the ground to ...

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Martian dust storm distribution and annual cycle from Mars daily global map observations

Wang

Saidel

Richardson

et al. 2023

Icarus

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Observations of Ubiquitous Nighttime Temperature Inversions in Mars' Tropics After Large‐Scale Dust Storms

Cited by 8 publications

References 33 publications

Mars Surface Pressure Oscillations as Precursors of Large Dust Storms Reaching Gale

Mars Surface Pressure Oscillations as Precursors of Large Dust Storms Reaching Gale

Gravity Waves in Different Atmospheric Layers During Martian Dust Storms

Martian dust storm distribution and annual cycle from Mars daily global map observations

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