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

  • Kohji Tomisaka
  • Masahiro N. Machida
  • Tomoaki Matsumoto
Chapter

Abstract

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.

Keywords

ISM: magnetic fields stars: formation ISM: jets and outflow stars: binary 

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Copyright information

© Springer Science+Business Media Dordrecht 2004

Authors and Affiliations

  • Kohji Tomisaka
    • 1
  • Masahiro N. Machida
    • 1
  • Tomoaki Matsumoto
    • 2
  1. 1.Theoretical AstrophysicsNational Astronomical ObservatoryMitaka, TokyoJapan
  2. 2.Faculty of Humanity and EnvironmentHosei UniversityFujimi, Chiyoda-ku, TokyoJapan

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