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Numerical Simulations of Collapse of a Magnetized Rotating Molecular Cloud

Published online by Cambridge University Press:  12 April 2016

Kanji Ohta  and
Asao Habe
Kanji Ohta
Affiliation:
Department of Physics, Hokkaido University, Sapporo, 060 JAPAN
Asao Habe
Affiliation:
Department of Physics, Hokkaido University, Sapporo, 060 JAPAN

Extract

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Recent observations reveal the velocity structure of star forming regions and the magnetic field in molecular clouds. It is known from observations that the molecular clouds rotate. It is suggested that the magnetic field have a important roll of the star formation process (e.g. Myers and Goodman 1988) and rotation of cloud have effects for evolution of molecular cloud. However it is not cleared how the magnetic field plays a roll of the star formation process in a rotating cloud.

In the previous theoretical studies, most of simulations are performed for collapse process of a rotating cloud without magnetic field (e.g. Miyama et al. 1984, Boss 1990) or collapse process of a magnetized cloud without rotation (e.g. Scott and Black 1980). Dorfi (1982) studied collapse of a magnetized, rotating cloud. However he did not calculate those with high resolutions, since he performed 3-dimensional calculations of about 6000 grid points.

Since observation instruments have been developed, it is possible to observe the star forming regions with good resolution. We study the collapse of the rotating, magnetized, isothermal cloud by mean of the axisymmetric numerical simulations with high resolution.

Type
3. Astronomical Results and Prospects
Information
International Astronomical Union Colloquium , Volume 140: Astronomy with Millimeter and Submillimeter Wave Interferometry , 1994 , pp. 280 - 281
Copyright
Copyright © Astronomical Society of the Pacific 1994

References

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