RADIATION MAGNETOHYDRODYNAMICS SIMULATION OF PROTO-STELLAR COLLAPSE: TWO-COMPONENT MOLECULAR OUTFLOW

Abstract

We perform a three-dimensional nested-grid radiation magneto-hydrodynamics\n(RMHD) simulation with self-gravity to study the early phase of the low-mass\nstar formation process from a rotating molecular cloud core to a first\nadiabatic core just before the second collapse begins. Radiation transfer is\nhandled with the flux-limited diffusion approximation, operator-splitting and\nimplicit time-integrator. In the RMHD simulation, the outer region of the first\ncore attains a higher entropy and the size of first core is larger than that in\nthe magnetohydrodynamics simulations with the barotropic approximation. Bipolar\nmolecular outflow consisting of two components is driven by magnetic Lorentz\nforce via different mechanisms, and shock heating by the outflow is observed.\nUsing the RMHD simulation we can predict and interpret the observed properties\nof star-forming clouds, first cores and outflows with millimeter/submillimeter\nradio interferometers, especially the Atacama Large Millimeter/submillimeter\nArray (ALMA).\n