a r t i c l e i n f o Amazonian non-polar ice deposits on Mars record periods and events when the climate differed substantially from that of today. Particularly evident are examples of ice-rich deposits in the martian mid-latitudes (lobate debris aprons, lineated valley fill, and concentric crater fill). Uncertain, however, is the amount of ice remaining in these deposits today, and the thickn...

Introduction: Impact crater clusters or crater strewn fields from primary impacts are found in MOC [1, 2], CTX, and HiRISE images [3, 4]. We present the analysis of new data on small craters and crater clusters accumulated by the HiRISE team for the first 10,000 orbits of MRO. New Craters on Mars: Repetitive imaging of Mars by various spacecraft revealed 20 potential " new " impact sites [2]: i...

Introduction: There are two important issues involving crater fluxes in the context of Callisto. First, there is the issue of establishing absolute crater fluxes, and several researchers have modeled absolute cratering fluxes of large craters on the Jovian Satellites [1]. Second, and the focus of the present study, is the issue of the lack of small craters relative to other crater sizes on Call...

Phase change and graphitization of diamonds from the Popigai impact crater (Krasnoyarsk Territory, Siberian platform, Russia) exposed to high-pressure high-temperature (HPHT) conditions 5.5 GPa 2000–2200 °C are studied by Raman spectroscopy X-ray diffractometry (XRD). Light-color type 1, free inclusions, with 0 10 % lonsdaleite, more resistant HPHT effects than dark 2 rich in lonsdaleite graphi...

Introduction: Most impact structures on Earth are modified by erosion. First order structural features of impact craters such as the crater diameter, the size of the central uplift, and ring syncline can be measured in field campaigns [e.g. 1] or by geophysical explorations [e.g. 2,3]. However, these quantities deviate from the original crater diameter or other morphological features of the pri...

2755. [19] Wieczorek, M. A. et al. (2013) Science 339, 671-675. Figure 1: Locations of floor-fractured craters [2] plotted on a basemap of crustal thickness [19]. Floor-fractured craters are preferentially located in regions of intermediate (20-30 km) crustal thickness. Mare deposits are located primarily on the lunar nearside and in regions of thinner crust. Figure 2: Crater Buch B (17.0°E, 39...

A hot and acid crater lake is located in the Nakadake crater, Aso volcano, Japan. The volume of water in the lake decreases with increasing activity, drying out prior to the magmatic eruptions. Salt-rich materials of various shapes were observed, falling from the volcanic plume during the active periods. In May 2011, salt flakes fell from the gas plume emitted from an intense fumarole when the ...

Crater Size-Frequency Distributions (SFD) on planetary surfaces are crucial to dating the geological age. On the Moon they have been employed together with radioactive K-Ar techniques to determine ages of different regions. The launch of the ESA Mars Express (MEX) mission on 6 June 2003 with the 9-view camera HRSC (High Resolution Stereo Camera) orbiting instrument and subsequent spectacular mu...

Endogenic modification in lunar floor-fractured craters can constrain spatial variations in early lunar conditions. The nature of these constraints, however, depends on the assumed mechanism of crater modification. For viscous relaxation, the extent of crater modification depends on the surrounding crustal viscosity and thus provides loose constraints on the history of crustal heating within a ...

The Chicxulub crater is the only wellpreserved peak-ring crater on Earth and linked, famously, to the K-T or K-Pg mass extinction event. For the first time, geologists have drilled into the peak ring of that crater in the International Ocean Discovery Program and International Continental Scientific Drilling Program (IODP-ICDP) Expedition 364. The Chicxulub impact event, the environmental calam...