Studies of the 2018/Mars Year 34 Planet‐Encircling Dust Storm

Guzewich, Scott D.; Fedorova, Anna; Kahre, M. A.; Toigo, A. D.

doi:10.1029/2020je006700

Cited by 16 publications

(6 citation statements)

References 52 publications

(131 reference statements)

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“…The hotter summer in the southern hemisphere, when Mars is closer to the Sun, increases the circulation and dust load in the atmosphere, warms it up, in turn increasing the dust uplift (Daerden et al, 2015). This positive feedback periodically, on average once every three Martian years, leads to global dust storms (GDSs) covering almost all tropical and midlatitudes (see, e.g., (Guzewich et al, 2020)). Historically, general circulation models describing the climate of Mars have used available measurements of atmospheric dust (Forget et al, 1999;Hartogh et al, 2005;Wilson and Hamilton, 1996).…”

Section: Scientific Objectives Related To the Atmospherementioning

confidence: 99%

Scientific Instrumentation Complex for the ExoMars-2022 Landing Platform

Korablev,

Rodionov,

Zelenyi

2024

Sol Syst Res

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Scientific objectives, instruments, and measurement program of the scientific instrumentation of the Kazachok stationary landing platform of the State Corporation Roscosmos and the European Space Agency (ESA) ExoMars-2022 project are presented. The scientific objectives of research on the landing platform included the long-term climate monitoring, the studies of the atmospheric composition, the mechanisms for dust lifting and related electrical phenomena, atmosphere–surface interactions, the subsurface water abundance, monitoring the radiation situation, and the study of Mars internal structure. To address these problems, 11 Russian and two European instruments with a total mass of 45 kg were built, tested and integrated into the spacecraft. These include a television camera system, meteorological complexes, a suite for studying dust and related electrical phenomena, optical spectrometers and an analytical complex for studying the atmospheric composition, a microwave radiometer, the neutron and gamma spectrometers for surface research, a seismometer, magnetometers and a Mars proper motion experiment to study its internal structure. Although the ExoMars-2022 project has been discontinued, the scientific objectives of the landing platform have not lost their relevance, and the technical solutions and developments implemented in scientific equipment are of interest and promising for further Mars exploration.

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Section: Scientific Objectives Related To the Atmospherementioning

confidence: 99%

Scientific Instrumentation Complex for the ExoMars-2022 Landing Platform

Korablev,

Rodionov,

Zelenyi

2024

Sol Syst Res

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“…In this regard, we follow the methodology of Fang et al (2021), except instead of focusing on a few dispersed intervals of time, we perform the fitting within sequential moving windows of fixed lengths of time throughout the time period of February 2015-February 2022. (Data during the 2018 dust storm MY = 34) are excluded; Guzewich et al, 2020. ) As shown in Figure 1, θ, LST, Ls, and F10.7 solar flux received at Mars (MF10.7) change continuously during the acquisition of data.…”

Section: Data Processingmentioning

confidence: 99%

Solar‐Synchronous Tides in Mars Thermosphere CO₂, Ar, and N₂ Densities From MAVEN

et al. 2023

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Measurements of CO2, Ar and N2 densities from the Neutral Gas and Ion Mass Spectrometer on the Mars Atmosphere and Volatile Evolution Mission (MAVEN) between 150 and 200 km altitude during 2015–2022 are analyzed to reveal diurnal (DW1), semidiurnal (SW2) and terdiurnal (TW3) solar‐synchronous tides in Mars thermosphere. Multi‐year‐mean tidal perturbations on a diurnal‐ and zonal‐mean background, corrected for solar flux variations, are reported as a function of latitude (48°S–48°N), altitude and solar longitude (Ls). The DW1, SW2 and TW3 amplitudes at for example, 180 km altitude are of order 90%–120%, 15%–20%, and ≲10% for CO2 and Ar, and roughly 2/3 these values for N2, the latter presumably due to the difference in molecular weight from the other species. Through examination of vertical phase progressions, DW1 is concluded to be mainly excited in situ, but SW2 and TW3 contain significant contributions from tides propagating upward from lower altitudes. By analogy with studies for Earth's thermosphere, the DW1 amplitudes and phases are thought to reflect the combined influences of thermal expansion and vertical winds. Points of agreement and disagreement with DW1, SW2, and TW3 amplitudes and phases derived from the Mars Climate Database are noted and interpreted.

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“…To the northeast of Hellas is Tyrrhena Terra, a part of the rugged and ancient, heavily cratered southern Martian highlands. Dust cover is very low throughout the region, although bright streaks show the direction of prevailing winds that have left dust deposits on the leeward side of nearly every crater rim in the area (Bennett et al., 2017; Guzewich et al., 2020). To the east of Tyrrhena Terra is Hesperia Planum, a broad lava plain in the southern highlands.…”

Section: Data Setmentioning

confidence: 99%

Constraining Changes in Surface Dust Thickness on Mars Using Diurnal Surface Temperature Observations From EMIRS

Wolfe,

Edwards,

Smith

et al. 2023

JGR Planets

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Diurnal surface temperature data collected from the Emirates Mars Infrared Spectrometer have been used to characterize dust redistribution on Mars following a regional dust storm in January 2022. A comparative temporal analysis is conducted pre‐ and post‐dust storm to estimate net changes in surface dust thickness at Syrtis Major, Isidis Planitia, Tyrrhena Terra, Hesperian Planum, and Elysium Planitia. By leveraging data from a numerical thermal model, we relate differences in observed surface temperature to changes in the thickness of the surface dust layer. We describe the methodology for estimating net changes in surface dust thickness, including a description of the thermophysical model employed, provide a sensitivity analysis with respect to local time and surface properties, and discuss the implications of our findings. Surface temperature differences suggest both dust deposition and removal, with some regions experiencing a net removal as high as 340 μm, while other regions experienced net deposition reaching up to 120 μm. Visible‐wavelength imagery from the Emirates Exploration Imager, which is more sensitive to changes in surface dust distribution, is incorporated in our analysis to provide additional context. When the area of each region of interest is accounted for, we find that the dust storm had the potential to remove and/or deposit more than 1.51 × 109 and 1.20 × 109 kg, respectively, suggesting that dust reservoirs are capable of transporting vast quantities of dust over short timescales.

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Studies of the 2018/Mars Year 34 Planet‐Encircling Dust Storm

Abstract: Spacecraft observations of martian "planet-encircling" or "global" dust storms extend back to Mariner 9, which famously arrived during the 1971 (Mars Year [MY] 9) global dust storm (GDS) and watched the storm decay from orbit (

Cited by 16 publications

References 52 publications

Scientific Instrumentation Complex for the ExoMars-2022 Landing Platform

Scientific Instrumentation Complex for the ExoMars-2022 Landing Platform

Solar‐Synchronous Tides in Mars Thermosphere CO₂, Ar, and N₂ Densities From MAVEN

Constraining Changes in Surface Dust Thickness on Mars Using Diurnal Surface Temperature Observations From EMIRS

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Studies of the 2018/Mars Year 34 Planet‐Encircling Dust Storm

Abstract: Spacecraft observations of martian "planet-encircling" or "global" dust storms extend back to Mariner 9, which famously arrived during the 1971 (Mars Year [MY] 9) global dust storm (GDS) and watched the storm decay from orbit (

Cited by 16 publications

References 52 publications

Scientific Instrumentation Complex for the ExoMars-2022 Landing Platform

Scientific Instrumentation Complex for the ExoMars-2022 Landing Platform

Solar‐Synchronous Tides in Mars Thermosphere CO2, Ar, and N2 Densities From MAVEN

Constraining Changes in Surface Dust Thickness on Mars Using Diurnal Surface Temperature Observations From EMIRS

Contact Info

Product

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Solar‐Synchronous Tides in Mars Thermosphere CO₂, Ar, and N₂ Densities From MAVEN