Magnetic fields and rotations of protostars

The early evolution of the magnetic field and angular momentum of newly formed protostars are studied, using three- dimensional resistive MHD nested grid simulations. Starting with a Bonnor- Ebert isothermal cloud rotating in a uniform magnetic field, we calculate the cloud evolution from the molecular cloud core (n(c) similar or equal to 10(4) cm(-3) and r = 4.6 x 10(5) AU, where n(c) and r are the central density and radius, respectively) to the stellar core (n(c) less than or similar to 10(12) cm(-3); r similar to 1 R-circle dot). The magnetic field strengths at the centers of clouds with the same initial angular momentum but different magnetic field strengths converge to a certain value as the clouds collapse for n(c) less than or similar to 10(12) cm(-3). For 10(12) cm(-3) less than or similar to n(c) less than or similar to 10(16) cm(-3), ohmic dissipation largely removes the magnetic field from a collapsing cloud core, and the magnetic field lines, which are strongly twisted for n(c) less than or similar to 101(2) cm(-3), are decollimated. The magnetic field lines are twisted and amplified again for n(c) greater than or similar to 10(16) cm(-3), because the magnetic field is recoupled with warm gas. Finally, protostars at their formation epoch (n(c) similar or equal to 10(21) cm(-3)) have magnetic fields of similar to 0.1-1 kG, which is comparable to observations. The magnetic field strength of a protostar depends slightly on the angular momentum of the host cloud. A protostar formed from a slowly rotating cloud core has a stronger magnetic field. The evolution of the angular momentum is closely related to the evolution of the magnetic field. The angular momentum in a collapsing cloud is removed by magnetic effects such as magnetic braking, outflow, and jets. The formed protostars have rotation periods of 0.1-2 days at their formation epoch, which is slightly shorter than observations. This indicates that a further removal mechanism for the angular momentum, such as interactions between the protostar and the disk, wind, or jets, is important in the further evolution of protostars.