Micro size craters were created by interaction of nanosecond laser beam with titanium target in liquid media. The dimension of crater i.e. depth and width is important in some applications such as micromachining. When the interaction occurs in liquid environment, the ablated materials from the target expand into the liquid. The ablated material can affect the interaction process if the ablated ...

Crater size–frequency analyses have shown that the largest volcanic plains deposits on Mercury were emplaced around 3.7 Ga, as determined with recent model production function chronologies for impact crater formation on that planet. To test the hypothesis that all major smooth plains on Mercury were emplaced by about that time, we determined crater size–frequency distributions for the nine next...

km in diameter. Although its orientation is roughly radial to Orientale, its morphology and setting imply that it may not be a secondary crater chain Crater chains, presumably formed by weak asteroids or com(Melosh and Whitaker 1994; Wichman and Wood 1995; Schenk et al. ets stretched apart by planetary tides, have been tentatively 1996). A second is the Abulfeda chain, which is *3.8 Gyr old, is...

The Boltysh crater has an entire suite of crater-fill impactites preserved, including two impact meltbearing breccias. Smectite occurrence in the breccias suggests two stages of alteration; an early hydrothermal mineralization, and a later, low temperature weathering. δD and δO of smectite separates are currently being measured and will be presented.

[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...

We performed numerical simulations of impact crater formation on Europa to infer the thickness and structure of its ice shell. The simulations were performed using iSALE to test both the conductive ice shell over ocean and the conductive lid over warm convective ice scenarios for a variety of conditions. The modeled crater depth-diameter is strongly dependent on the thermal gradient and tempera...

Introduction: Previous studies describe the evolution of impact generated vapor plumes from above [1]. Here, a new approach is tested whereby early-time self-luminous ejecta products are examined using quarter-space experiments with spectral measurements. At early times, the forming cavity is on the order of centimeters. Hence, the pointing accuracy and small detection regions are necessary. Th...

Introduction. The Mjølnir submarine crater (40 km in diameter and located in the Barents Sea) is interpreted as formed by the impact of an 1.5 to 2 km in diameter asteroid [1,2] into a 200–400 m deep epicontinental paleo-Barents Sea [3]. The target area consisted of a sedimentary sequence of Devonian to Jurassic age, at least 6 km thick, overlying older, well lithified sedimentary strata. The s...

Introduction: Transient and disruption cavity sizes are fundamental parameters in the study of impact structures [1]. They are governed by the velocity, size and density of the impacting body, the target density and ambient gravitational acceleration. Hence, knowledge of transient and disruption cavity dimensions allows the calculation of energy release associated with impact. Since the recogni...

Introduction: It has been estimated that the total number of meteoroids entering the Earth's atmosphere with masses above 1 kg is about 37000 per year [1]. And approximately 4400 events with mass more than 1 kg strike the Earth every year [1]. Among these im-pactors, those in the mass range ~10 4-3.10 6 kg fragment and form crater fields, with the largest crater resulting from impact of the lar...