Properties and effects of dust particles suspended in the Martian atmosphere

Abstract

Direct measurements of the optical depth above the two Viking landers are reported for a period covering the summer, fall, and winter seasons in the northern hemisphere, a time period during which two global dust storms occurred. The optical depth had a value of about 1 just before the onset of each storm; it increased very rapidly, on a time scale of a few days, to peak values of about 3 and 6 with the arrival of the first and second storms, respectively; and it steadily decreased shortly thereafter (≳ few days to few weeks) for both storms, with the decay occurring more rapidly during the initial period of decay. We have also carried out further analyses of observations of the sky brightness made with the lander cameras during the summer season to obtain improved estimates of other dust particle parameters, including the cross section weighted mean particle radius, several shape factors, and the imaginary indices of refraction. These results have been used to define the radiative properties of the suspended dust particles at solar wavelengths. Particle properties inferred by Toon et al. (1977) from their study of the Mariner 9 Iris data were employed to define the radiative properties of the dust at thermal wavelengths. In an effort to understand the effect of dust content on atmospheric temperatures and winds, we have incorporated the derived radiative properties of the dust into a 1 D radiative convective model. When only radiation and thermal convection are taken into account, these calculations fail to reproduce the temperature structure determined during the descent of the landers to the surface. However, satisfactory agreement is achieved when allowance is made for the effects of vertical motions induced by large scale atmospheric dynamics. The sign and magnitude of the required vertical velocities are crudely consistent with those found by Pollack et al. (1976a) in their general circulation calculations. The diurnal temperature variations predicted by the 1 D calculations for the observed optical depths are also in crude agreement with values inferred from orbiter and lander measurements. The 1 D model predicts that the diurnal temperature change and daily mean temperature, averaged over the entire atmospheric vertical column, steadily increase as the optical depth of the dust increases to a value of several, and then subsequently change little. Thus, for small and moderate values of optical depth, there is a positive feedback between atmospheric dust content and both tidal and seasonal winds, but little feedback occurs for very large values of optical depth. A negative feedback exists between dust content and thermally driven topographic winds. The occurrence of these feedback effects are supported by several Viking observations. It is suggested that they play a role in the generation of certain types of local dust storms, in the development of local dust storms into global ones, and in the decay of global storms. At present, dust is being preferentially deposited in the north polar region due to scavan...

THEMIS VIS and IR observations of a high‐altitude Martian dust devil

“…Additionally, the surface evolution of Mars is currently dominated by the atmospheric dust cycle, which governs the rate of exhumation, transportation, and deposition of dust on the surface [Christensen and Moore, 1992;Thomas and Gierasch, 1985]. Regional and global dust storms were originally assumed to dominate this cycle, but Pollack et al [1979] showed that dust settles from the atmosphere too rapidly after such events to account for the continuous opacity caused by suspended particles. Dust devils have been shown to help maintain this perennial atmospheric haze [Fisher et al, 2005], and are important mechanisms for redistributing substantial amounts of the Martian surface over short geological time periods [Ringrose et al, 2003].…”

Seasonal variation of aerosols in the Martian atmosphere

“…Sun at various zenith angles in the broadband solar channel centered on 670 nm [Pollack et al, , 1979Colburn et al, 1989]. These are shown in Plates la and ld.…”

“…The current standard view of the dust cycle derives from Viking Lander (VL) measurements of the visible optical depth since the optical depth of the atmosphere provides a measure of the amount of suspended aerosols. The key assumption in the interpretation of these data has been that only dust significantly contributes to the daytime opacity [Pollack et al, 1979;Colburn et al, 1989] and hence that the amount of atmospheric dust can be directly derived from them. However, dust is not the only Copyright 2000 by the American Geophysical Union.…”

Color and albedo of the south polar layered deposits on Mars

“…The lower portion of the mosaic, where the layered deposits appear, was corrected for atmospheric scattering (Plate 2) and used to create the R/V mosaic shown in Figure 2. The atmospheric brightness and attenuation at selected points in the mosaic were predicted using 2.5-tz radius particles [Pollack et al, 1979] with the scattering properties given in Table 2. The best fit model (normal optical depth = 0.13) was run at 35 points in a 400 x 400 pixel grid; then bilinear interpolation was used to approximate the atmospheric brightness and attenuation at every other pixel in each color mosaic.…”