DATING VOLCANISM AND RIFTING ON VENUS USING IMPACT CRATER DENSITIES

Although the distribution of impact craters on Venus is indistinguisha ble from a completely spatially random population on the basis of crat er data alone, the addition of geologic information indicates that the craters are not random with respect to geology. Areas of low crater d ensity correlate with concentrations of tectonic and volcanic features , as well as high proportions of faulted and embayed craters. High-res olution mapping of large volcanoes, flood-type lava flow fields, rifts , and coronae shows that these features have low crater densities that are unlikely to have occurred merely by chance. Because these feature s also appear young based on stratigraphic data, difference in age is the most likely reason for differences in crater density between geolo gically defined terrains. Crater densities may be used to determine re liable relative ages for sufficiently large geologic terrains containi ng at least eight to nine craters, as long as the mapping criteria are independent of impact crater locations. This result provides a tool t o begin identifying and dating major geologic provinces, and to begin developing a geologic history of Venus. Using a simple data model, and calculating crater ages relative to an assumed global mean age of 300 Ma, we show that the ages of large volcanoes (72+/-45 Ma), now fields (128+/-91 Ma), rifts (130+/-145 Ma), and coronae (120+/-115 Ma) are a ll substantially younger than the mean plains age, and probably repres ent ongoing volcanic and tectonic activity, rather than the end of a b rief global resurfacing event with a mean age of 300 Ma.