First MHD Simulation of Collapse and Fragmentation of Magnetized Molecular Cloud Cores

Details First MHD Simulation of Collapse and Fragmentation of Magnetized Molecular Cloud Cores First MHD Simulation of Collapse and Fragmentation of Magnetized Molecular Cloud Cores

2003-11-14

arxiv.org/abs/astro-ph/0311339v2

Mon.Not.Roy.Astron.Soc. 348 (2004) L1

Astronomy and Astrophysics

Astrophysics

Accepted by MNRAS Letters, 6 pages, 2 figures. A high resolution version may be found at http://astro3.sci.hokudai.ac.jp/~ma

Scientific paper

10.1111/j.1365-2966.2004.07402.x

This is the first paper about the fragmentation and mass outflow in the molecular cloud by using three-dimensional MHD nested-grid simulations. The binary star formation process is studied paying particular attention to the fragmentation of a rotating magnetized molecular cloud. We assume an isothermal rotating and magnetized cylindrical cloud in hydrostatic balance. Non-axisymmetric as well as axisymmetric perturbations are added to the initial state and the subsequent evolutions are studied. The evolution is characterized by three parameters: the amplitude of the non-axisymmetric perturbations, the rotation speed, and the magnetic field strength. As a result, it is found that non-axisymmetry hardly evolves in the early phase, but begins to grow after the gas contracts and forms a thin disk. Disk formation is strongly promoted by the rotation speed and the magnetic field strength. There are two types of fragmentation: fragmentation from a ring and that from a bar. Thin adiabatic cores fragment if a thickness is smaller than 1/4 of the radius. For the fragments to survive, they should be formed in a heavily elongated barred core or a flat round disk. In the models showing fragmentation, outflows from respective fragments are found as well as those driven by the rotating bar or the disk.

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