Gravitational Contraction of Magnetized Clouds

Abstract

In this paper, the dynamical contraction of magnetized clouds is studied from the run-away phase to the accretion phase throughout. Since the non-homologous gravitational contraction necessitates progressively finer spatial resolution, “nested grid technique” (Burger & Oliger 1984) is adopted. As a result, it is found that outflow driven by toroidal magnetic fields is occurred in the accretion phase, which explains molecular outflows in protostellar objects (see also Tomisaka 1998). In contrast, a rotationally supported disk is formed in a cloud core without magnetic fields.