Impact craters are used for a wide array of investigations planetary surfaces. A crater form that is somewhat rare, forming only ∼10% impact craters, the polygonal (or PIC). These have been visually, manually identified as having at least two rim segments best represented straight lines. Such lines or edges most often to infer details about subsurface crust where faults control structure cavity...

Introduction: Populations of impact craters are widely used in planetary science to study surface ages and the nature of resurfacing. Apparent surface age depends on scale; at smaller scales natural surfaces tend to be younger. High resolution imaging of Mars has revealed that at the scales of decameters and smaller, surprisingly many different terrains are devoid of small craters and hence are...

Introduction: The Kara River basin, located between the Pai-Khoi ridge and the Baydarata Gulf of the Kara Sea 200 km to the north of Vorkuta, Russia, was found to be an impact structure in 1970’s [1,2]. The 40Ar-39Ar impactite ages vary from 70 to 75 Ma [3,4]. Actually, two craters were suggested [1]: The Kara crater, 60-65 km in diameter, was defined on the Kara River estuary while the 25 km U...

During space exposure solar cell arrangements and cover shields of satellites are subject to intense bombardement by natural and man-made debris which causes impact craters and other damage on the surfaces. In order to calibrate particle impact properties of retrieved material a number of defined projectiles were shot under controlled conditions at samples of solar cells and thermal Multi-Layer...

[1] Data from the Mars Orbiter Laser Altimeter (MOLA) and Mars Orbiter Camera (MOC) instruments aboard the Mars Global Surveyor (MGS) were used in a detailed search of a selected part of the South Polar Layered Deposits (SPLD) for impact craters. Impact craters with diameters from 0.8 to 5 km were identified from a MOLA-derived shaded relief map and were primarily validated using individual MOL...

[1] The density of impact craters calibrated against lunar data is currently the only quantitative measure of surface age for terrestrial planetary surfaces. Unlike the Moon, however, Mars has been weathered and eroded, obliterating some small (<10 km diameter) craters, a phenomenon addressed in the Mariner/Viking days of Mars exploration but commonly overlooked in recent studies. We present a ...

We undertook a photogeologic study of Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) images of the ejecta of the very young 22-km diameter crater Giordano Bruno (GB) and for the Luna 24 landing site region, where secondary craters from Giordano Bruno are observed. Using the technique of Basilevsky (1976) for estimating the absolute ages of small lunar craters based on thei...

Some fresh impact craters on Ganymede have the overall ejecta morphology similar to Martian double-layer ejecta (DLE), with the exception of the crater Nergal that is most like Martian single layer ejecta (SLE) craters (as is the terrestrial crater Lonar). Similar craters also have been identified on Europa, but no outer ejecta layer has been found on these craters. The morphometry of these cra...