The Ensemble Mars Atmosphere Reanalysis System (EMARS) Version 1.0

Greybush, Steven J.; Kalnay, Eugenia; Wilson, R. J.; Hoffman, Ross N.; Nehrkorn, T.; Leidner, M.; Eluszkiewicz, J.; Gillespie, H. E.; Wespetal, M.; Zhao, Yongjing; Hoffman, Matthew J.; Dudas, Patrick M.; McConnochie, T. H.; Kleinböhl, A.; Kass, D. M.; McCleese, D. J.; Miyoshi, Takemasa

doi:10.1002/gdj3.77

Cited by 40 publications

(60 citation statements)

References 56 publications

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“…The results presented here show how varied the nighttime atmosphere in the dusty season can be, and how there is an important interplay between the dust distribution, water ice clouds and thermal tides. The diurnal temperature behavior and vertical dust distribution revealed in these MCS observations is not well represented in assimilated datasets of the martian atmosphere (Greybush et al., 2019; Holmes et al., 2020) and suggests further work is needed in order to understand the coupling between the dust and water cycles.…”

Section: Resultsmentioning

confidence: 92%

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

Steele

Kleinboehl

Kass

2021

Geophysical Research Letters

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We report the ubiquitous occurrence of nighttime temperature inversions in the tropical Martian atmosphere during the dusty season, as observed by the Mars Climate Sounder. The inversions occur after large‐scale regional dust storms, with their strengths largely correlated to the strengths of the dust storms. Inversions strengthen between 2 and 4 a.m., with the bases of the inversions getting cooler, and the tops of the inversions getting warmer. The inversions are strongest and most frequent around Tharsis and Terra Sabaea, but are also observed over the flat plains early in the dust storm decay period. These inversions likely result from the effects of both a strengthened migrating diurnal tide (due to the increased dustiness of the atmosphere), along with nonmigrating tides forced by zonal variations in aerosol abundance and topography. These results highlight an important interplay between the dust distribution, water ice clouds and thermal tides.

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Section: Resultsmentioning

confidence: 92%

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

Steele

Kleinboehl

Kass

2021

Geophysical Research Letters

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“…Indeed the present paper suggests that assimilation of MCS‐like middle‐atmosphere measurements into a whole‐atmosphere Mars model could represent a leap forward in our ability to predict thermosphere longitude structures due to solar tides. While significant advances have been made insofar as data assimilation of low‐ and middle‐atmosphere data goes (Greybush et al, 2019; Navarro et al, 2017), it remains to be determined how thermosphere structures are affected. Concerning the need for future observations, major advances would likely result from improved local time sampling of Mars atmosphere.…”

Section: Discussionmentioning

confidence: 99%

Solar Tides in the Middle and Upper Atmosphere of Mars

et al. 2020

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Solar tides are responsible for much of the spatial-temporal variability of Mars' upper atmosphere (100-∼200 km). However, the tidal spectrum, its latitude versus Ls variability, and its vertical evolution remain uncertain. In this paper, Mars Climate Sounder temperature measurements at 76 km above Mars' areoid are used to construct a multiyear latitude versus Ls climatology of the tidal spectrum. The most important spectral components include the solar-synchronous ("migrating") components DW1, SW2, and the solar-asynchronous ("nonmigrating") tides DE3, DE2, DE1, SE1, S0, and SW1. The Mars Climate Database (MCD), which provides predictions from the Laboratoire de Météorologie Dynamique Global Climate Model, captures particularly well the amplitudes and key structural features of the solar-asynchronous tides at 76 km that furthermore underly the large longitudinal structures in density that are observed between 100 and 200 km. Height-latitude and latitude-Ls structures of MCD density perturbations are therefore examined between 76 and 172 km and interpreted in terms of mean wind and dissipation effects. In particular, due to the smaller radius and more intense zonal-mean zonal winds at Mars compared to Earth, Doppler-shift effects are significantly exaggerated compared to Earth. Evidence is also provided for nonnegligible contributions to density variability from stationary planetary waves which arise from tide-tide nonlinear interactions. It is moreover shown that MCD captures the salient amplitude and phase characteristics of the ∼±30-60% longitudinal density perturbations measured by the Mars Global Surveyor accelerometer. This, and the excellent MCD-MCS agreement at 76 km, lends credibility to the ability of MCD to provide new insights into thermosphere density variability at Mars due to vertical coupling by solar tides. where t = universal time (UT), Ω = 2 sol −1 , z = altitude, = latitude, integer s is the zonal wavenumber, integer n defines the frequency or period of the oscillation, A n, s is the amplitude, and n, s is the phase

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“…In order to test the hypothesis that downwelling associated with the diurnal tide can cause the temperature inversions observed in the MCS measurements, we use Ensemble Mars Atmosphere Reanalysis System (EMARS) version 1.0 data (Greybush et al, 2019) for MY29. This data set results from the assimilation of MCS in-track temperature profiles using a Local Ensemble Transform Kalman Filter (LETKF; see Hoffman et al, 2010;Greybush et al, 2012;Zhao et al, 2015), and is freely available at https://www.datacommons.…”

Section: Appendix A: Temperature Inversions In Emars Datamentioning

confidence: 99%

Aerosols and Tides in the Martian Tropics During Southern Hemisphere Spring Equinox From Mars Climate Sounder Data

et al. 2021

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Thermal tides are global-scale oscillations of atmospheric temperature, pressure and wind, which are sub-harmonics of a solar day. They are driven by solar heating of the atmosphere and surface, and due to Mars' thinner atmosphere they play a much more significant role than on Earth. They can influence surface pressure and wind, affect the transport of aerosols, and propagate into the upper atmosphere (Forbes, 2002;

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The Ensemble Mars Atmosphere Reanalysis System (EMARS) Version 1.0

Cited by 40 publications

References 56 publications

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

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

Solar Tides in the Middle and Upper Atmosphere of Mars

Aerosols and Tides in the Martian Tropics During Southern Hemisphere Spring Equinox From Mars Climate Sounder Data

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