Abstract
The remnant magnetization of chondrite type meteorite matter indicates the existence of 10 −5–10 −3 T magnetic fields in the early Solar System accretion disk. Taking into account parameter regimes being typical for this evolutionary stage of Sun and planets we consider the protosolar disk matter as partially ionized dusty plasma consisting of massive charged dust grains, neutral gas, electrons and ions. Results of systematic multifluid neutral gas–plasma–dust simulations show that shear flow driven collisional interactions yield a self-magnetization of the early Solar System matter which is able to explain the measured remnant magnetization of meteorite material.
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