Fig. 5. Dusty olivines as carriers of nebular magnetization.

(A) Reflected light optical photomicrograph of dusty olivine-bearing chondrule in the LL Semarkona meteorite. Light gray regions are mostly forsterite, whereas darker gray regions outlined by white dashed lines are rich in dusty metal. (B) Transmission electron microscopy image of four dusty olivine kamacite crystals (white ellipsoids) in forsterite (dark gray background). (C) Relaxation times at room temperature of kamacite cuboids with aspect ratios of 1.5 as calculated by micromagnetic modeling and compared to the age of the solar system (gray line). Grains larger than 25 nm in diameter are in the single vortex state, while smaller grains are in the uniform (e.g., single domain or flower) state. (A) and (B) after (10) and (C) after (130). Photo credit for (A): R. R. Fu, MIT.