Natalia Artemieva

TL;DR: A 10-km diameter impact crater named Zunil in the Cerberus Plains of Mars created ∼ 10 7 secondary craters 10 to 200 m in diameter as discussed by the authors, which are concentrated in radial streaks that extend up to 1600 km from the primary crater, identical to lunar rays.

TL;DR: In this paper, the authors review the presently available data sets in support of this paradigmatic assumption, as follows: (1) the phenomenology of lunar impact craters, (2) the terrestrial record of the impact cratering process and the interpretation of terrestrial impactites as far as this “ground truth” is relevant for the interpretation, and (3) the theory and numerical simulation of the cratering processes and the characteristics of the Earth-Moon crossing population of impactors (asteroids and comets), the principles of relative age dating of lunar surface units and the

TL;DR: Artemieva et al. as mentioned in this paper investigated the transfer of meteorites from Mars to Earth with a combined mineralogical and numerical approach and used quantitative shock pressure barometry and thermodynamic calculations of post-shock temperatures to constrain the pressure/temperature conditions for the ejection of Martian meteorites.

TL;DR: In this article, the authors studied the production of potential martian meteorites numerically within the frame of 3D hydrodynamic modeling and found that the ratio of the volume of escaping solid ejecta to projectile volume depends on the impact angle, impact velocity and the volatile content in the projectile and in the target.

TL;DR: In this paper, a variety of 2D and 3D codes were used in this study, from commercial products like AUTODYN, to codes developed within the scientific community like SOVA, SPH, ZEUS-MP, iSALE, and codes developed at U.S. National Laboratories like CTH, SAGE/RAGE, and ALE3D.