Radar Doppler Spectroscopy of Mars: elevation differences between bright and dark areas. I, Volume 1An analysis of radar observations of Mars, particularly at 12.5-cm wavelength, performed at the Goldstone facility of the Jet Propulsion Laboratory, during the 1965 opposition. Then the entire range of Martian longitudes at North latitude 21.6° was observed with an effective topographical resolution in the quasi-specular component of some 6 planetocentric degrees. |
Common terms and phrases
15 toward observer 1963 radar swath 1965 Goldstone 1965 opposition Aeria Aethiopis AMAZONIS areas are highlands Arecibo backscatter bandpass Carl Sagan centered central frequency central spike Ceraunius Cerberus contribute correlation degrees Deuteronilus diffuse component Doppler Dyce Earth elevation differences Elysium Figure Goldstein high radar reflectivity High-frequency asym higher longitudes Jet Propulsion Laboratory Kotelnikov latitude longitude displacement longitude strips Low-frequency asym low-frequency asymmetry low-frequency tail lowlands Martian cartography Martian dark areas Martian longitude mean slope metry of centroid Meudon Observatories Moab Moeris Lacus Nepenthes Niliacus Lacus Nilokeras Nix Olympica North American Aviation observations of Mars optical dark areas planetocentric Pollack probable error properly aligned radar observations radar return radar-reflectivity maxima reflectivity maxima regions of high required slopes Sagan secular changes slopes of Syrtis Smithsonian Astrophysical Observatory spectra spectral features spectrogram specular reflection subterrestrial point Symmetrical quasi-specular component Syrtis Major Table topographical resolution total power Tractus Albus Xanthe