Mars aerosol studies with the MGS TES emission phase function observations: Optical depths, particle sizes, and ice cloud types versus latitude and solar longitude

By R. Clancy, Michael J. Wolff, Philip R. Christensen. 2003

306 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/047dd413fe7bb3ea21cadcefe181e609c8d95554

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Citations in the corpus

Temperature inversions, thermal tides, and water ice clouds in the Martian tropics (2003, methodology): “This value is consistent with recent observations [e.g., Pearl et al., 2001; Clancy et al., 2003; Wolff and Clancy, 2003; Glenar et al., 2003].”
CRISM multispectral summary products: Parameterizing mineral diversity on Mars from reflectance (2007, background): “Figure 13 shows a longitudinally averaged seasonal plot of the parameter R410, the reflectance at 0.41 mm. This parameter succeeds as an indicator for the aphelion cloud belt at subtropical northern latitudes, as well as bright topographic clouds and high-altitude hazes [ Clancy et al., 1996, 2003 ]”
Dust aerosol, clouds, and the atmospheric optical depth record over 5 Mars years of the Mars Exploration Rover mission (2014, background): “This pattern is similar to patterns reported by Clancy et al. (2003) using orbital infrared spectroscopy, and generally consistent with dust sizes of 1.2–1.4 lm Please cite this article in press as: Lemmon, M.T., et al. Dust aerosol, clouds, Exploration Rover mission.”
Origin and role of water ice clouds in the Martian water cycle as inferred from a general circulation model (2004, background): “Although current estimates of cloud particle size are very sparse and restricted to a few regions and seasons, they already exhibit significant variations between northern summer and other seasons [Clancy et al., 2003].”
Mars Climate Sounder: An investigation of thermal and water vapor structure, dust and condensate distributions in the atmosphere, and energy balance of the polar regions (2007, methodology): “TES data shows indications of subtle changes in the dust spectral shape attributed to particle size changes [Wolff and Clancy, 2003] that appear to be associated primarily with dust storms, but also have a seasonal dependence [ Clancy et al., 2003 ].”
Interannual variability in TES atmospheric observations of Mars during 1999–2003 (2004, methodology): “In addition to thermal infrared spectra, the TES instrument can also observe the visible/near-infrared solar reflectance at 0.3–2.9 µm giving a measurement of visible albedo (Kieffer et al., 2000; Christensen et al., 2001; Clancy et al., 2003 ).”
Constraints on dust aerosols from the Mars Exploration Rovers using MGS overflights and Mini‐TES (2006, methodology): “Although the concept of the EPF was introduced during the Viking Orbiter mission to study the directional dependence of surface thermal emission processes, it is better known for its utility in aerosol characterization studies [Kieffer et al., 1976; Clancy and Lee, 1991; Clancy et al., 2003b ].”
Constraints on the size of Martian aerosols from Thermal Emission Spectrometer observations (2003, methodology): “Very consistent aerosol size distributions are obtained when 9 mm dust and 12 mm ice optical depths retrieved from this analysis are compared to visible optical depths retrieved from TES solar band emission phase function sequences [Clancy et al., 2003].”
Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO) (2007, methodology): “In addition, such retrievals will form the basis of atmospheric ‘‘correction’’ re-processing for the multispectral survey (initial processing will be done with climatological data based on observations from MGS TES [Smith, 2004]).”
THE MARTIAN ATMOSPHERIC BOUNDARY LAYER (2011, background): “[60] The types of surface‐based remote sensing instruments flown to date include imaging systems, LIDARs, and Thermal Emission Spectrometers (TESs).”
Wavelength dependence of dust aerosol single scattering albedo as observed by the Compact Reconnaissance Imaging Spectrometer (2009, methodology): “The differences in the I/F for ‘‘negative’’ and ‘‘positive’’ emergence angles is an illustration of the functional differences in the effective scattering by the atmosphere and surface, as was recognized in previous EPF analyses [e.g., Clancy and Lee, 1991; Clancy et al., 2003a ].”
Modeling the Martian dust cycle and surface dust reservoirs with the NASA Ames general circulation model (2006, methodology): “The single scattering albedo employed in the model is 0.86 [Pollack et al., 1979, 1990], which is low based on more recently derived values from TES [Wolff and Clancy, 2003; Clancy et al., 2003 ].”
Compact Reconnaissance Imaging Spectrometer observations of water vapor and carbon monoxide (2009, background): “The typical EPF sequence includes 11 images, with five taken inbound at emission angles between roughly 30 and 70, one image taken at nadir (near zero emission angle as MRO passes over the site), and five more images taken outbound at emission angles between roughly 30 and 70. The purpose of the EPF”
Observations of the south seasonal cap of Mars during recession in 2004–2006 by the OMEGA visible/near‐infrared imaging spectrometer on board Mars Express (2007, background): “However, this is not a critical issue for the relatively small grained surface H2O frost ( 100 mm) which is typical of seasonal caps, and this approach minimizes the impact of aerosol diffusion, which is characterized by a blue slope in this wavelength range [Clancy et al., 2003].”
Mars Climate Sounder limb profile retrieval of atmospheric temperature, pressure, and dust and water ice opacity (2009, methodology): “Analyses of the size distribution of water ice particles based on MGS TES data give reff = 1–2 mm for ice hazes between 20 and 40 km altitude and reff = 3–4 mm in the aphelion cloud belt [Wolff and Clancy, 2003; Clancy et al., 2003].”
Spacecraft Observations of the Martian Atmosphere (2008, methodology): “…wavelengths of 9 and 20 microns (e.g., Wolff & Clancy 2003 for TES observations), or between infrared (9 microns) and visible wavelengths (e.g., Clancy et al. 2003 for TES observations; Lemmon et al. 2004, Wolff et al. 2006 for MER observations), give useful constraints on particle size, which…”