Introduction: The discovery of a secondary-crater strewn field generated by the 10-km crater Zunil [1] stirred up a discussion of what is the real shape of the primary production crater size-frequency distribution and if age determination based on craters in the smaller-crater size range is possible. The main point of the discussion is whether or not the steep branch (below about 1 km diameter)...

The location of Meteor Crater is shown on nearly all highway maps of Arizona. It lies 6 mi (9.7 km) south of 1-40 between Flagstaff and Winslow in northern Arizona; the turnoff from 1-40, 34 mi (55 km) east of Flagstaff, is well marked by signs along the highway. Access to the crater is by a paved road that leads directly to a visitor center and museum on the rim of the crater. Qualified scient...

available online at http://meteoritics.org 1331 © The Meteoritical Society, 2006. Printed in USA. Geological and geochemical data from the proposed Sirente crater field: New age dating and evidence for heating of target Jens ORMÖ1*, Christian KOEBERL2, Angelo Pio ROSSI3, 4, and Goro KOMATSU3 1Centro de Astrobiología (CSIC/INTA), Instituto Nacional de Técnica Aeroespacial, Ctra de Torrejón a Aja...

Introduction: Terby impact crater is located at the northeastern part of Hellas region (75°E – 30°S) on the cratered highlands. Using multi-dataset available on this area, we investigated the geological story of Terby crater. MOLA altimetry [1] shows that Terby impact crater displays an anomalous morphology compared to other impact crater of ~200 km in diameter. Instead of a circular depression...

Introduction: The Bosumtwi Impact Crater in Ghana, Africa (6°32’N, 1°25’W) is a large complex crater. The crater is 10.5 km in diameter, with a central uplift 2 km in diameter. It is the source of the Ivory Coast Tektite field, found to the southwest of the crater over 200 km away. This study investigates the mineralogy, the petrology, and the geochemistry of drill core samples taken near the c...

Introduction: The 22 km ∅ crater “Giordano Bruno” is the youngest lunar crater of its size or larger [1]. The crater is located at 36N / 103E in the Th-poor lunar highlands and has a prominent ejecta ray system. According to urban ledgend formation of the Giordano Bruno crater was observed by medieval monks on June 18, 1178 A.D [2]. However, formation of a 22 km sized crater on the Moon would...

Introduction: The geometries of simple impact craters reflect the properties of the target materials, and the diverse range of fluidized morphologies observed in Martian ejecta blankets are controlled by the near surface composition and the climate at the time of impact. Using the Mars Orbiter Laser Altimeter data set, quantitative information about the strength of the upper crust and the dynam...

Carbonate samples from the 8.9-Mt nuclear (near-surface xplosion) crater, OAK, and a terrestrial impact crater, Meteor Crater, were analyzed for shock damage using electron paramagnetic resonance (EPR). Samples from below the OAK apparent crater floor were obtained from six boreholes, as well as ejecta recovered from the crater floor. The degree of shock damage in the carbonate material was ass...

Unlike other types of fluidized ejecta impact craters, Martian double-layered ejecta (DLE) craters rarely have secondary impact craters [1]. In our continued effort to understand DLE and other types of Martian fluidized ejecta craters we have examined recently acquired THEMIS images, and found two exceptionally fresh DLE craters that include well-developed secondary crater fields. One of these ...

[1] The 750 m diameter and 75 m deep Victoria crater in Meridiani Planum, Mars, is a degraded primary impact structure retaining a 5 m raised rim consisting of 1–2 m of uplifted rocks overlain by 3 m of ejecta at the rim crest. The rim is 120–220 m wide and is surrounded by a dark annulus reaching an average of 590 m beyond the raised rim. Comparison between observed morphology and that expecte...