The Martian Dichotomy: Numerical Investigations of the Impact Hypothesis

Details The Martian Dichotomy: Numerical Investigations of the Impact Hypothesis The Martian Dichotomy: Numerical Investigations of the Impact Hypothesis

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p34b..07h&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P34B-07

Physics

5400 Planetary Sciences: Solid Surface Planets, 5420 Impact Phenomena, Cratering (6022, 8136)

Scientific paper

The Martian dichotomy is a first order feature of Martian topography and crustal thickness distribution [1]. We examine the hypothesis that a single large impact may have caused the dichotomy [2,3], using the radially- axisymmetric hydrocode ZeusMP [4,5]. We use a variable-resolution Eulerian grid to resolve near-surface processes, and have incorporated a set of Lagrangian tracer particles to track the displacement of crustal material allowing for robust crater size determination. We have explored parameter space by varying both impact velocity and mass, and have derived a preliminary scaling law for the amount of crustal material removed. The pattern of energy deposition is also being studied to better understand the spatial distribution of melted and excavated material. [1]Zuber, M.T., Nature 412, 220-27, 2001. [2]Willhelms, D.E., S.W. Squyres, Nature 309, 138-40, 1984. [3]Marinova, M.M., O. Aharonson, E. Asphaug 2005, Eos Trans. AGU, 86(52), Fall Meet. Suppl., Abstract P42A-06 [4]Stone, J. and M. Norman 1992, Ap. J. Supp. vol. 80, 753-790. [5]Korycansky, D. G., Zahnle, K. J., and M.-M. Mac Low 2000. Icarus, vol. 146, 387-403

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