Radar studies of the Martian surface at centimeter wavelengths - The 1975 opposition

Details Radar studies of the Martian surface at centimeter wavelengths - The 1975 opposition Radar studies of the Martian surface at centimeter wavelengths - The 1975 opposition

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978icar...33..441d&link_type=abstract

Icarus, vol. 33, Mar. 1978, p. 441-453.

Astronomy and Astrophysics

Astronomy

3

Centimeter Waves, Doppler Radar, Mars Surface, Radar Astronomy, Radar Maps, Continuous Radiation, Radar Scattering, Viking Lander 1, Wavelengths, Centimeter Waves, Mars, Surface, Radar, Schiaparelli, Syrtis Major, Meridiani Sinus, Spectrum, Radar Profiling, Morphology, Reflectivity, Opposition, Doppler Navigation Experiment

Scientific paper

The Goldstone radar system was operated at wavelengths of 3.5 and 12.6 cm to probe the Martian surface during the 1975 opposition. Regions studied in detail by range-Doppler techniques are Syrtis Major, Sinus Meridiani, and the crater Schiaparelli. Average rms slopes of 1.6 and 1.1 deg were measured in Syrtis Major at 3.5 and 12.6 cm, respectively, while the average reflectivity was about 0.064 at both wavelengths. No wavelength dependence of surface roughness was seen in Sinus Meridiani, where rms surface slopes averaged 1.8 deg and the reflectivity was about 0.08. The regions around Schiaparelli were probed at a 12.6-cm wavelength. The echo from the bottom of the crater was undetectable. Operating at 3.5 cm during May and June of 1976, 149 CW echo spectra were obtained near latitude 18 deg, sampling most longitudes including the early Viking landing sites. The average total radar cross section is 4.8% of the geometrical cross section. The diffuse component was estimated to be 1.9%, leaving 2.9% to the average quasi-specular component. The average rms slope is 4.1 deg.

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