DISSIPATION OF MAGNETIC FIELDS IN STAR-FORMING CLOUDS WITH DIFFERENT METALLICITIES

We study the dissipation process of magnetic fields in the metallicity range 0-1Z(circle dot) for contracting prestellar cloud cores. By solving non-equilibrium chemistry for important charged species, including charged grains, we evaluate the drift velocity of the magnetic-field lines with respect to the gas. We find that the magnetic flux dissipates in the density range 10(12) cm(-3) less than or similar to n(H) less than or similar to 10(17) cm(-3) for the solar-metallicity case at the scale of the core, which is assumed to be the Jeans scale. The dissipation density range becomes narrower for lower metallicity. The magnetic field is always frozen to the gas below metallicity less than or similar to 10(-7)-10(-6) Z(circle dot), depending on the ionization rate by cosmic rays and/or radioactivity. With the same metallicity, the dissipation density range becomes wider for lower ionization rates. The presence of such a dissipative regime is expected to cause various dynamical phenomena in protostellar evolution such as the suppression of jet/outflow launching and the fragmentation of circumstellar disks depending on the metallicity.