The First Two Thousand Years of Star Formation

Abstract

Starting from a prestellar core with a size of $1.2\times 10^4$ AU, we calculate the evolution of a gravitationally collapsing core until $\sim 2000$ yr after protostar formation using a three-dimensional resistive magnetohydrodynamic simulation, in which the protostar is resolved with a spatial resolution of $5.6\times 10^{-3}$ AU. Following protostar formation, a rotationally supported disk is formed. Although the disk size is as small as $\sim 2-4$ AU, it remains present until the end of the simulation. Since the magnetic field dissipates and the angular momentum is then not effectively transferred by magnetic effects, the disk surface density gradually increases and spiral arms develop due to gravitational instability. The disk angular momentum is then transferred mainly by gravitational torques, which induce an episodic mass accretion onto the central protostar. The episodic accretion causes a highly time-variable mass ejection (the high-velocity jet) near the disk inner edge, where the magnetic field is well coupled with the neutral gas. As the mass of the central protostar increases, the jet velocity gradually increases and exceeds $\sim 100$ km s${}^{-1}$. The jet opening angle widens with time at its base, while the jet keeps a very good collimation on the large scale. In addition, a low-velocity outflow is driven from the disk outer edge. A cavity-like structure, a bow shock and several knots, all of which are usually observed in star-forming regions, are produced in the outflowing region.

arXiv comment31 pages, 13 figures, Accepted for publication in ApJ

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