Contraction and Fragmentation of Magnetized Rotating Clouds and Formation of Binary Systems

Details Contraction and Fragmentation of Magnetized Rotating Clouds and Formation of Binary Systems Contraction and Fragmentation of Magnetized Rotating Clouds and Formation of Binary Systems

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ap%26ss.292..309t&link_type=abstract

Astrophysics and Space Science, v. 292, Issue 1, p. 309-316 (2004).

Astronomy and Astrophysics

Astrophysics

Ism: Magnetic Fields, Stars: Formation, Ism: Jets And Outflow, Stars: Binary

Scientific paper

Using three-dimensional (3D) magnetohydrodynamical (MHD) nested-grid simulations, the fragmentation of a rotating magnetized molecular cloud core is studied. An isothermal rotating magnetized cylindrical cloud in hydrostatic balance is considered. We studied non-axisymmetric evolution of the cloud. It is found that non-axisymmetry hardly evolves in the early phase, but it begins to grow after the gas contracts and forms a thin disk. The disk formation and thus growth of non-axisymmetric perturbation are strongly promoted by rotation and magnetic field strength. We found two types of fragmentations: fragmentation from a ring and that from a bar. These two types of fragmentations occur in thin adiabatic cores with the thickness being smaller than 1/4 of the radial size. 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 that driven by the rotating bar or the disk.

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