Radar characteristics of small craters - Implications for Venus

Details Radar characteristics of small craters - Implications for Venus Radar characteristics of small craters - Implications for Venus

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987em%26p...37...89g&link_type=abstract

Earth, Moon, and Planets (ISSN 0167-9295), vol. 37, Jan. 1987, p. 89-111.

Astronomy and Astrophysics

Astronomy

7

Earth Surface, Planetary Craters, Radar Imagery, Shuttle Imaging Radar, Venus Surface, Earth Observations (From Space), Magellan Ultraviolet Astronomy Satellite, Minerals, Radar Data, Rayleigh Scattering, Solar System, Volcanoes

Scientific paper

Shuttle radar images (SIR-A) of volcanic and impact craters were examined to assess their appearance on radar images. Radar characteristics were determined for (1) nine maarlikie craters in the Pinacate volcanic field, Sonora, Mexico; (2) the caldera of Cerro Volcan Quemado, in the Bolivian Andes; (3) Talemzane impact crater, Algeria; and (4) Al Umchaimin, a possible impact structure in Iraq. SIR-A images were compared with conventional photographs and with results from field studies. Consideration was then given to radar images available for Venus, or anticipated from the Magellan mission. Of the criteria ordinarily used to identify impact craters, some can be assessed with radar images and others cannot be used; planimetric form, expressed as circularity, and ejecta-block distribution can be assessed on radar images, but rim and floor elevations relative to the surrounding plain and disposition of rim strata are difficult or impossible to determine. It is concluded that it will be difficult to separate small impact craters from small volcanic craters on Venus using radar images and is suggested that it will be necessary to understand the geological setting of the areas containing the craters in order to determine their origin.

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