Self-Magnetization of the Early Solar System Matter

The remnant magnetization of chondrite type meteorite matter indicates the existence of 10^-5 - 10^-3 Tesla magnetic fields in the early solar system accretion disk. Taking into account parameter regimes being typical for this early evolutionary stage of the partially ionized dusty proto-solar accretion disk we performed self-consistent three-dimensional multi fluid plasma - neutral gas - dust simulations. The results of our systematic simulations show that shear flow driven collisional interactions are able to yield self-induced magnetic fields of the order of 10^-5 - 10^-3 Tesla in a dusty proto-planetary accretion disk on very short time scales of the order of a few years. Thus, shear flow induced self-magnetization can yield a significant contribution to the magnetization of the early solar system and is able to explain the measured remnant magnetization of meteorite material.