Vertical structure and size distributions of Martian aerosols from solar occultation measurements

Abstract

Solar occultations performed with a spectrometer on board the Soviet spacecraft Phobos 2 (Blamont et al. 1991) provided data on the vertical structure of the Martian aerosols in the equatorial region (0°–20° N latitude) near the northern spring equinox ( L S = 0°–20°). All measurements were made close to the evening terminator. Five clouds were detected above 45 km altitude and their vertical structure recorded at six wavelengths between 0.28 and 3.7 μm. They have a small vertical extent (3–6 km) and a vertical optical depth less than 0.03. The thermal structure, as derived from saturated profiles of water vapor observed by our instrument in the infrared, does not allow the CO 2 frost point to be reached at cloud altitude, strongly suggesting that cloud particles are formed of H 2O ice. Under the assumption of spherical particles, a precise determination of their effective radius, which varies from cloud to cloud and with altitude, is obtained and ranges from 0.15 to 0.85 μm; an estimate of the effective variance of the particle size distribution is ∼ 0.2. The number density of cloud particles at the peak extinction level is ∼1 cm −3. Dust was also observed and monitored at two wavelengths, 1.9 and 3.7 μm, on nine different occasions. The top of the dust opaque layer, defined as the level above which the atmosphere becomes nearly transparent at the wavelengths of observation, is located near 25 km altitude, with variations smaller than ±3 km from place to place. The scale height of dust at this altitude is 3–4 km. The effective radius of dust particles near the top of the opaque layer is 0.95 ± 0.25 μm and increases below with a vertical gradient of ∼0.05 μm km −1. Assuming that particles are levitated by eddy mixing, the eddy diffusion coefficient, K, is found to be ∼10 6 cm 2 sec −1 at 25 km and 10 5−10 6 cm 2 sec −1 at 50 km using, respectively, dust and cloud observations. An effective variance of 0.25 (±50%) for the dust size distribution is obtained on the basis of a simple theoretical model for the observed vertical gradient of the effective radius of dust particles. Three clouds observed by Viking at midlatitude during the northern summer are reanalyzed. The analysis gives K ≈ 10 6 cm 2 sec −1 below 50 km altitude and at least 10 7 cm 2 sec −1 above. Since the clouds seen from Phobos 2 are observed at twilight, which coincides with the diurnal maximum of the ambient temperature, they can be assumed to be in a steady state. If their thermodynamic state were to vary quickly during the day, our optical thickness at twilight would correspond to unrealistic values in earlier hours when the temperature is lower. Clouds are well fitted by theoretical profiles obtained assuming the steady state. An atmospheric temperature of 165–170 K at ∼50 km is inferred. The negative temperature gradient above the cloud is large (1.5–2 K km −1). A parallel is established between these thin clouds and the polar mesospheric clouds observed on Earth. It is shown that upwelling in equatorial regions at equinox could be a significant factor in levitating cloud particles.