Complex refractive index of Martian dust: Mariner 9 ultraviolet observations

Pang, Kevin D.; Ajello, J. M.; Hord, C. W.; Egan, Walter G.

doi:10.1016/0019-1035(76)90184-6

Cited by 42 publications

(21 citation statements)

References 26 publications

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“…It was found that photometric and polarimetric observation as a function of the phase angle, depends on hypothesis about the particle structure [ Dlugach et al , 2002]. In the same way, Pang et al [1976] fitting the backscattering peak of the dust phase function with Mie theory found micron‐sized particles. Later, Chýlek and Gramm [1978] using a model of scattering by irregular particles, but using a composite phase function (from two data sets taken at two separate sites) found submicronic particle radii.…”

Section: Resultsmentioning

confidence: 97%

Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM

Rannou¹,

Perrier²,

Bertaux³

et al. 2006

J. Geophys. Res.

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The UV detector of Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars (SPICAM) on board Mars Express has measured several profiles of light scattered at the limb of Mars. In this paper we present 33 profiles taken between January 2004 and August 2005. Scattering of UV light at the limb of Mars is due to the molecules of the atmosphere, dust particles, and sometimes cloud particles which appear as detached layers above the extended dust layer. We have used a radiative transfer model to retrieve the haze and cloud properties. Rough estimate of the particle size shows that both cloud particles and dust particles above 20 km are in the range 10 to 100 nm. Such particles are much smaller than micron-sized dust particles previously observed in the lower atmosphere, generally from landers. Gravitational segregation is thought to be responsible for these differences in particle size between low and high atmosphere

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Section: Resultsmentioning

confidence: 97%

Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM

Rannou¹,

Perrier²,

Bertaux³

et al. 2006

J. Geophys. Res.

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“…On the other hand, the paucity of similar retrievals relevant to Bands 6 and 7 simplifies the situation. The most relevant comparison is with the results of Pang et al (1976). They find an imaginary index (k) of 0.02 at 268 nm and 0.01 at 305 nm.…”

Section: Refractive Indicesmentioning

confidence: 95%

“…The combination of limb viewing observations as well as the global dust event of 1971 stimulated several investigations, including those involving non-spherical particle effects Ajello et al, , 1976Pang et al, 1976;Chý lek and Grams, 1978). The next 30 years contains scattered efforts using data from a variety of sources such as the Orbiting Astronomical Observatory 2 (Caldwell, 1977), Mars-5 (Krasnopolskii et al, 1980), and the Hubble Space Telescope (e.g., James et al, 1994;Clancy et al, 1996;Goguen et al, 2003).…”

Section: Introductionmentioning

confidence: 97%

Ultraviolet dust aerosol properties as observed by MARCI

Wolff

Clancy

Goguen

et al. 2010

Icarus

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“…However, the agreement between the published Viking [ Pollack et al , 1995] and the Pathfinder [ Tomasko et al , 1999] retrievals is interpreted by some as an indication that the size has remained constant between the two epochs [e.g., Tomasko et al , 1999; Smith and Lemmon , 1999]. Although the earlier Mariner 9 dust storm retrievals of much smaller and larger sizes [ Pang et al , 1976; Toon et al , 1977] are considered problematic due to model approximations and assumptions [see Clancy et al , 1995], the similarity of the Viking and Pathfinder retrievals represents only three spatial locations with limited temporal coverage. Clearly, more work can be done.…”

Section: Introductionmentioning

confidence: 99%

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

2003

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[1] We combine a robust multiple-scattering radiative transfer algorithm with the Thermal Emission Spectrometer (TES) spectral data set in order to characterize the properties of Martian aerosol particles. Because of the importance of accurate model input when performing such retrievals, we include self-consistent and physically plausible treatments of surface emissivity and atmospheric aerosol dielectric functions, as well as gaseous absorption effects. Considerable effort is expended in the identification and discussion of potential sources of error and uncertainty. Significant results stemming from this analysis are a new dust aerosol dielectric function that appears to well represent the IR spectral behavior sampled by TES for a wide range of dust loading conditions, two distinct populations of water ice particles with r eff of $1-2 mm and $3-4 mm; and distinct departures in dust particle sizes during the 2001A global dust storm from the canonical 1.6-1.7 mm values. 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]. Direct comparison of our optical depths to those available from the Planetary Data System (PDS) (as provided by the TES science team) reveals a systematic bias toward t values which are 20-30% (or more) too small. Much of this offset stems from the fact that TES PDS aerosol optical depths are actually an approximation to t absorption , which is $30% lower than t extinction for Mars dust aerosols. Additional biases in TES optical depths arise from assumptions of fixed surface emissivity and temperature.

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Complex refractive index of Martian dust: Mariner 9 ultraviolet observations

Cited by 42 publications

References 26 publications

Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM

Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM

Ultraviolet dust aerosol properties as observed by MARCI

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

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