New 3.5-cm wavelength radar images of the equatorial regions of Mercury

Details New 3.5-cm wavelength radar images of the equatorial regions of Mercury New 3.5-cm wavelength radar images of the equatorial regions of Mercury

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28..687j&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 687.

Computer Science

Radar Imagery, Mercury Surface, Equatorial Regions, Doppler Radar, Radar Tracking

Scientific paper

Delay-Doppler radar observations in 1996 presented the opportunity to examine terrain on both the imaged and unimaged hemispheres of Mercury. However, the analysis of delay-Doppler radar data in heavily cratered terrain requires a more complicated fitting process than for Venus, where the terrain is mostly flat. Because of these difficulties, the measurements of the Fresnel reflection constant, the Hagfors scattering constant, and the ranges determined along the 'Doppler equator' have larger formal (and actual) errors than the parameters determined from smooth terrain. Advances in real-time signal processing have allowed us to cover 2-3 times more range than in previous observations. Improvements in the sensitivity of the Goldstone radar during the past five years permit the greater coverage in range and also allow useful observations of Mercury at distances as great as 1.2 AU. Radar reflectivity images obtained near close Earth-approach (inferior conjunctions) often have coverage as large as 15 to 20 deg from the subearth point. Even though these single-receiver images have the usual delay-Doppler north-south ambiguities, such images reveal the type of terrain, the crater density, and the small-scale roughness of the region imaged. Radar observations extend our knowledge of the surface of Mercury into the hemisphere unphotographed by Mariner 10. (Abstract only)

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