Workshop on Issues in Crater Studies and the Dating of Planetary Surfaces (2015) 9051.pdf CHALLENGES USING SMALL CRATERS FOR DATING PLANETARY SURFACES. J.-P. Williams1 and A. V. Pathare2, 1Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA 90095 (
[email protected]), 2Planetary Science Institute, Tuscon, AZ 85719 (
[email protected]). Introduction: Impact craters can be used to esti- mate the age of a planetary surface, given knowledge of the rate of crater accumulation, and are the primary method for age dating planetary surfaces (excluding Earth) (e.g. [1][2]). The factors shaping crater produc- tion at diameters < 100 m are not well understood and under debate. However, because of the frequency at which these craters form, they are utilized to discrimi- nate surface ages of geologically young regions and features at a higher spatial resolution. This level of resolution is required to establish the temporal relation of recent geologic activity on the Moon such as Co- pernican impacs, including North Ray, South Ray, and Cone craters, sites used to anchor the crater chronolo- Fig 1. Impact melt deposit on the ejecta of Giordano gy, and Mars such as gully, landslide, and outflow Bruno crater and crater SFD on and off of the melt channel formation, volcanic resurfacing, sedimenta- deposit with nominal lunar regolith and hard rock tion, exhumation, dune activity, glaciation and other isochrons [7]. periglacial landforms, and the possible relation of such 7 features to obliquity variations of ~10 y timescale. Self-Secondary Craters: The melt deposit also il- Radiometric and cosmic ray exposure ages of lustrates another issue that may confound crater count- Apollo and Luna samples, correlated with crater popu- ing on the ejecta of craters.