Looking for Martian True Polar Wander in mutually oriented slices of ALH84001

True polar wander (TPW) on Mars has been hypothesized based on a variety of observations including geoid instability [1], locations of apparent polar deposits [2], and locations of magnetic anomalies [3, 4]. A proposed driving force for TPW is redistribution of mass on the surface of the planet such as by extensive volcanism events [5]. The majority of TPW modeling research has been using orbital datasets and modeling. However, laboratory analyses of Martian samples should also be conducted to test for Martian TPW. The Martian meteorite, ALH84001, is a prime sample for observing Martian TPW because of its preservation of thermal remanent magnetization from Mars [6]. Previous work on the sample has demonstrated that the interior of the meteorite was not heated above 40 C during transport from Mars to Earth and that there is a heterogeneous magnetization within the meteorite [7]. Within the meteorite are a series of fracture-filling carbonate blebs which contain magnetite and pyrrhotite with original remanence. These carbonates are presumed to have precipitated onto the meteorite [8]. We have divided a fracture-containing portion of the meteorite into three sets of sequential, mutually oriented slices. Using an ultra-high resolution scanning SQuID magnetometer we are able to visualize the magnetization within each slice. We are able to model each magnetic scan as a series of discrete dipoles using a modification from Lima and Weiss [9]. Our results demonstrate that within one of our slice sequences the dipoles lie along a great circle path. Dipoles lying along an arc in a stereographic projection can be interpreted as resulting from TPW if there is a significant amount of time from start to end of magnetization. Our ongoing work includes continued analysis and scanning of our slices as well as statistical tests for confirming if the dipoles lie along an arc. [1] Sprenke, KF et al. 2005 Icarus 174(2) 486-9 [2] Perron, JT et al. 2007 Nature 447(7146) 840-3 [3] Kobayashi, D & Sprenke, KF 2010 Icarus 210(1) 37-42 [4] Boutin, D & Arkani-Hamed, J 2006 Icarus 181(1) 13-25 [5] Kite, ES et al. 2009 Earth Planet Sci Lett 280(1-4) 254-67 [6] Weiss, B et al. 2000 Science 290(5492) 791-5 [7] Weiss, BP et al. 2002 Earth Planet Sci Lett 201(3-4) 449-63 [8] Halevy, I et al. 2011 Proc Natl Acad Sci 108(41) 16895-9 [9] Lima, EA & Weiss, BP 2009 J Geophys Res 114(B6)