Most meteorites originate from small planetary bodies (<500 km radius) formed within the first million years (Myr) of the solar system (Wright & Grady, 2006). The existence of iron and stony-iron meteorites indicates that part of these bodies underwent large-scale differentiation (Elkins-Tanton et al., 2011;McCoy et al., 2006), possibly generating planetary magnetic fields by dynamo processes due to convection of molten metallic cores (Bryson et al., 2015;Nichols et al., 2016). Recent paleomagnetic studies in (stony-)iron meteorites suggest that these materials can preserve magnetic records of planetary fields generated by their parent bodies (Maurel et al., 2020;Nichols et al., 2016Nichols et al., , 2021. Extracting paleomagnetic records from early solar materials is contingent on the presence of magnetic minerals capable of preserving magnetization states over solar system timescales. Taenite and tetrataenite are ferromagnetic minerals commonly observed in (stony-)iron meteorite groups-for example, IIEs