Magnetic and microstructural characterisation of FeNi: Insight into the formation and impact history of the IAB parent body

The IABs represent one of only two groups of iron meteorites that did not form by fractional crystallization of liquid Fe-Ni in the core of a differentiated planetesimal. Instead, they are believed to originate from a partially differentiated body that was severely disrupted by one or more impacts during its early history. Paleomagnetic signals from two IABs, Toluca and Odessa, were investigated using X-ray magnetic circular dichroism (XMCD) and X-ray photoemission electron microscopy (X-PEEM) to image the magnetisation of the cloudy zone. The IABs do not appear to have experienced a magnetic field, consistent with the lack of a metallic core on the parent body. We also present a detailed microstructural and magnetic study of the observed FeNi microstructures, characterising their properties using XMCD and X-PEEM. The crystallographic architecture of the microstructures was analysed using electron backscatter diffraction (EBSD). Odessa and Toluca both exhibit a complex series of microstructures, requiring an unusual evolution during slow cooling. A conventional Widmanstätten sequence of kamacite, tetrataenite rim and cloudy zone developed via slow cooling to temperatures below 400 ºC. Subsequent modification of the microstructures resulted in the formation of pearlitic plessite and spheroidized plessite. Compositional and crystallographic analysis suggests that pearlitic and spheroidized plessite formed by impact modification of the cloudy zone and martensite, respectively. This study highlights the importance of characterising microstructures in order to corroborate paleomagnetic observations, as well as improving our understanding of the processes effecting planetary formation and evolution.