Lacustrine sediments from the 24 km diameter Boltysh impact structure record the rapid formation of an intra-crater lake. Stable isotope compositions and organic maturity parameters from the lake sediments deposited post-impact show that they were heated by underlying impactites. This heating is attributed to the establishment of an impactgenerated hydrothermal system. Estimates of the duration...

crops of parautocthonous megabreccia (MBu) in Uzboi Valles ~x km from the rim of Holden crater. PARAUTOCHTHONOUS MEGABRECCIAS AND POSSIBLE EVIDENCE OF IMPACT-INDUCED HYDROTHERMAL ALTERATION IN HOLDEN CRATER, MARS. L. L. Tornabene, G. R. Osinski, and A. S. McEwen, Lunar and Planetary Lab, University of Arizona, 1541 E. University Blvd., Tucson, Arizona, 85721, USA ([email protected], De...

Introduction: Isidis Planitia, a Noachian impact crater infilled with Hesperian aged basalts, is located on Mars on the crustal dichotomy and is antipodal to the Tharsis rise [1]. Measuring 1400 km across and 2 km deep, it is comparable in scale and age to lunar mascons. The basin contains an interesting pattern of both radial and concentric wrinkle ridges (see Figure 1), and massive graben are...

Because of atmospheric shielding and endogenic resurfacing, the population of impact craters on Venus is small (about a thousand) and consists of large craters. This population has been used in numerous studies with the goal of deciphering the geologic and geodynamic history of Venus, but the nearly spatially random nature of the crater population has complicated efforts to understand this hist...

Introduction: Crater ejecta launched from the surface of small, rapidly-rotating, and highly-elongated and irregularly-shaped bodies are subjected to a complex dynamical process. Dynamical models [1,2] of reaccretion of impact ejecta on asteroids provide important tools for a detailed investigation of the distribution of blocks and finer regolith across Eros’ surface as revealed by the NEAR MSI...

Introduction: Giordano Bruno (GB) crater is among the youngest large lunar impact craters (22 km diameter at 36°N, 103°E (Fig. 1)). Its crisp morphology, extensive ray system, and spectral properties imply a young age (<<1 by). Spectral data [1, 2] indicate the ray material is immature having an optical maturity index, calculated from the Clementine 950/750 nm ratio [2, 3] of ~0.27. It was sugg...

[1] Analysis of high resolution Moon Mineralogy Mapper (M) data reveals the presence of a prominent Mg‐spinel‐rich lithology in the central peaks of Theophilus crater on the lunar nearside. Other peak‐associated lithologies are comprised of plagioclase, olivine, and pyroxene‐bearingmaterials. A consistent spatial association of Mg‐spinel with mafic‐free anorthosite is recognized. Documentation ...

525 © Meteoritical Society, 2001. Printed in USA. Abstract–It has been suggested that the formation of the 22 km diameter lunar crater Giordano Bruno was witnessed in June 1178 A.D. To date, this hypothesis has not been well tested. Such an impact on the Earth would be "civilization threatening". Previous studies have shown that the formation of Giordano Bruno would lead to the arrival of 10 mi...

Gale Crater contains Mount Sharp, a ~5km thick stratigraphic record of Mars’ early environmental history. The strata comprising Mount Sharp are believed to be sedimentary in origin, but the specific depositional environments recorded by the rocks remain speculative. We present orbital evidence for the occurrence of eolian sandstones within Gale Crater and the lower reaches of Mount Sharp, inclu...