Constraints on the size of Martian aerosols from Thermal Emission Spectrometer observations

By Michael J. Wolff, R. Clancy. 2003

239 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/f23a5d5ec07fdfa1fb5f15308a4e9ce27723fa6f

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Citations in the corpus

Apparent thermal inertia and the surface heterogeneity of Mars (2007, background): “On the other hand, Wolff and Clancy (2003) and Smith (2004) point out that the TES-derived atmospheric dust opacities are likely to underestimate extinction by 20–30%, and are actually more consistent with absorption opacities.”
One Martian year of atmospheric observations using MER Mini‐TES (2006, methodology): “, 2001] has been used extensively to retrieve the spatial and temporal variations of atmospheric temperatures and aerosol properties from orbit [e.g., Conrath et al., 2000; Wolff and Clancy, 2003; Smith, 2004].”
Revisiting the radiative impact of dust on Mars using the LMD Global Climate Model (2011, background): “Wolff et al. [2009] extend this latter coverage to 4 mm through the MEX‐ OMEGA observations of Määttänen et al.”
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].”
Subvisible CO2 ice clouds detected in the mesosphere of Mars (2006, background): “Our particle radius estimates are based on the measurement of the spectral slope of aerosol extinction, a forward scattering quantity almost independent of aerosol morphology (as recently reviewed by Wolff and Clancy, 2003).”
Constraints on dust aerosols from the Mars Exploration Rovers using MGS overflights and Mini‐TES (2006, methodology): “We employ the same algorithm to describe the observational errors as in our earlier work [Wolff and Clancy, 2003, section 3]: the NESR values (for a single detector, 2.5 10 8 W cm 2 sr 1 cm 1 from 300 cm 1 to 1400 cm 1; 6 10 8 W cm 2 sr 1 cm 1 at 250 cm 1; 4 E12S17 WOLFF ET AL.”
The influence of radiatively active water ice clouds on the Martian climate (2012, background): “Since the focus of this paper is the radiative effect of clouds, cloud opacities and particle sizes were compared to TES and OMEGA observations [Smith, 2004; Wolff and Clancy, 2003; Madeleine et al., 2012] to ensure that heating rates are accurate.”
Eight-year climatology of dust optical depth on Mars (2014, background): “Secondly, it converts full-extinction IR values to absorption-only at 9.3 lm by dividing by a factor 1.3 (Smith, 2004; Wolff and Clancy, 2003).”
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].”
Wavelength dependence of dust aerosol single scattering albedo as observed by the Compact Reconnaissance Imaging Spectrometer (2009, methodology): “Using the refractive indices from the reff =1 .8mm case, as motivated by the discussion in section 5.1, we compute the aerosol scattering properties for a particle size representative of diffuse dust loading, reff =1 .4mm [e.g., Wolff and Clancy, 2003; Lemmon et al., 2004; Wolff et al., 2006; Sode”
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].”
Spacecraft Observations of the Martian Atmosphere (2008, methodology): “…spectra taken as emission-phase functions (EPF), where a fixed spot of the surface is viewed at a wide range of emission angles as an orbiting spacecraft passes over the spot, has been used by Wolff & Clancy (2003) to find an average value of reff = 1.5–1.6 µm, consistent with lander results.”
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.”
Interannual variability in TES atmospheric observations of Mars during 1999–2003 (2004, background): “Although recent work by Clancy et al. (2003) and Wolff and Clancy (2003) show that both dust and ice can have small variations in their spectral dependence, and that these differences are detectable in TES spectra, our analysis shows that their effect on retrieved optical depth is relatively small”
T-matrix theory of electromagnetic scattering by particles and its applications: a comprehensive reference database (2004, background): “…(1975) Warner and Hizal (1976) Waterman (1971) Waterman (1979) Wauben et al. (1993) Whitney andWolff (2002) Wielaard et al. (1997) Wirth et al. (1999) Wolff and Clancy (2003) Wong et al. (2004) Wriedt and Doicu (1998b) Xing and Greenberg (1994a) Xing and Greenberg (1994b) Yeh et al. (1982b)…”
Mars aerosol studies with the MGS TES emission phase function observations: Optical depths, particle sizes, and ice cloud types versus latitude and solar longitude (2003, methodology): “In these cases, aerosol particle sizes independently determined from quantitatively accurate visible/IR optical depth ratios (here) and IR spectral fits [Wolff and Clancy, 2003] are compared, providing particularly sensitive definitions of particle size variations among Mars ice and dust aerosols.”