The distribution, composition, and particle properties of Mars mesospheric aerosols: An analysis of CRISM visible/near-IR limb spectra with context from near-coincident MCS and MARCI observations

Clancy, R. T.; Wolff, Michael; Smith, M. D.; Kleinböhl, A.; Cantor, B. A.; Murchie, S. L.; Toigo, A. D.; Seelos, K. D.; Lefèvre, Franck; Montmessin, Franck; Daerden, F.; Sandor, Brad J.

doi:10.1016/j.icarus.2019.03.025

Cited by 49 publications

(120 citation statements)

References 65 publications

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“…We observe that the particle size decreases on average with increasing altitude (cf. Figure ), as previously reported by Clancy et al (). This global trend is also apparent in the majority of individual profiles: particle size is observed to decrease with altitude within a given cloud as we can see in Figure .…”

Section: Resultssupporting

confidence: 89%

“…As the main cloud altitude increases, water ice particles become distinctly smaller in the storm, with a median effective radius of

0.28 normalμ

m before the dust storm and

\leq

0.1

normalμ

m during it. This narrower range of smaller particles, with a strong peak for

r_{eff} \leq 0.2 normalμ

m, is typical of the mesospheric clouds (Clancy et al, , Figure ).…”

Section: Resultsmentioning

confidence: 79%

“…However, high‐cloud altitudes are nearly systematic in our observations during the peak phase of the GDS (cf. Figure ), while such altitudes are less typical during non‐GDS years (Clancy et al, ). Moreover, peak cloud altitudes are slightly higher during the onset of the GDS than reported in non‐GDS years.…”

Section: Resultsmentioning

confidence: 93%

“…These high‐altitude water ice clouds are observed only at the beginning of the GDS. High‐altitude water ice clouds can also be seen during non‐dust GDS years, when they occur during the storm season (Clancy et al, ; Vincendon et al, ). However, high‐cloud altitudes are nearly systematic in our observations during the peak phase of the GDS (cf.…”

Section: Resultsmentioning

confidence: 99%

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Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

et al. 2020

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The Atmospheric Chemistry Suite (ACS) instrument onboard the ExoMars Trace Gas Orbiter (TGO) European Space Agency‐Roscosmos mission began science operations in March 2018. ACS Mid‐InfraRed (MIR) channel notably provides solar occultation observations of the Martian atmosphere in the 2.3‐ to 4.2‐ normalμ m spectral range. Here, we use these observations to characterize water ice clouds before and during the MY 34 Global Dust Storm (GDS). We developed a method to detect water ice clouds with mean particle size ≤ 2 normalμ m and applied it to observations gathered between Ls=165∘ and Ls=243∘. We observe a shift in water ice cloud maximum altitudes from about 60 km before the GDS to above 90 km during the storm. These very high altitude, small‐sized ( reff≤0.3.3emnormalμ m) water ice clouds are more frequent during MY 34 compared to non‐GDS years at the same season. Particle size frequently decreases with altitude, both locally within a given profile and globally in the whole data set. We observe that the maximum altitude at which a given size is observed can increase during the GDS by several tens of kilometers for certain sizes. We notably notice some large water ice particles ( reff≥1.5.3emnormalμ m) at surprisingly high altitudes during the GDS (50–70 km). These results suggest that GDS can significantly impact the formation and properties of high‐altitude water ice clouds as compared to the usual perihelion dust activity.

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Section: Resultssupporting

confidence: 89%

“…As the main cloud altitude increases, water ice particles become distinctly smaller in the storm, with a median effective radius of

0.28 normalμ

m before the dust storm and

\leq

0.1

normalμ

m during it. This narrower range of smaller particles, with a strong peak for

r_{eff} \leq 0.2 normalμ

m, is typical of the mesospheric clouds (Clancy et al, , Figure ).…”

Section: Resultsmentioning

confidence: 79%

Section: Resultsmentioning

confidence: 93%

Section: Resultsmentioning

confidence: 99%

See 2 more Smart Citations

Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

et al. 2020

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“…If these clouds formed a uniform layer above the planet and crossed the planet's shadow, the greatest minimum illuminated altitude is their maximum altitude. If this assumption is reasonable, these altitudes rule out a

normal C O_{2}

‐ice composition because

normal C O_{2}

‐ice clouds normally form at altitudes higher than 50 km and the increased warming from the global dust storm makes their formation more implausible (Clancy & Sandor, ; Clancy et al, ).…”

Section: Twilight Cloud Observationsmentioning

confidence: 99%

Mars's Twilight Cloud Band: A New Cloud Feature Seen During the Mars Year 34 Global Dust Storm

Connour

Schneider

Milby

et al. 2020

Geophysical Research Letters

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We report a new water‐ice cloud feature observed during the Mars year 34 global dust storm: twilight cloud bands that routinely formed just past the evening terminator. We use images taken by the MAVEN/IUVS instrument. These bands were often latitudinally continuous, spanning over 6,000 km and were present between 18:00 and 19:00 local time. They were present for nearly the entire time IUVS imaged the evening terminator and often reached altitudes of at least 40 to 50 km during the mature phase of the storm. We compare these observations to LMD global climate model simulations. The simulations generally contain the temporal and spatial extents of the bands seen in IUVS data throughout the storm, but there are some discrepancies. We infer that these clouds formed as a result of semidiurnal thermal tides.

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Vertical aerosol distribution and mesospheric clouds from ExoMars UVIS

Streeter

Sellers

Wolff

et al. 2021

Preprint

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Suspended atmospheric aerosols are key components of the martian atmosphere, and their vertical distribution has long been a subject of investigation with orbital observations and modeling. The aerosols found in Mars' atmosphere are mineral dust, water ice, and CO 2 ice, and each have distinct spatiotemporal distributions and radiative effects. Early analytical calculations based on estimated dust sedimentation and diffusion rates alongside orbital observations of a Global Dust Storm (GDS) led to the development of a standard dust profile often used

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The distribution, composition, and particle properties of Mars mesospheric aerosols: An analysis of CRISM visible/near-IR limb spectra with context from near-coincident MCS and MARCI observations

Cited by 49 publications

References 65 publications

Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

Martian Water Ice Clouds During the 2018 Global Dust Storm as Observed by the ACS‐MIR Channel Onboard the Trace Gas Orbiter

Mars's Twilight Cloud Band: A New Cloud Feature Seen During the Mars Year 34 Global Dust Storm

Vertical aerosol distribution and mesospheric clouds from ExoMars UVIS

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