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Self-Gravitational Instability of an Isothermal Gaseous Slab under High External Pressure

Published online by Cambridge University Press:  13 May 2016

Michihisa Umekawa ,
Ryoji Matsumoto ,
Shigeki Miyaji  and
Tatsuo Yoshida
Michihisa Umekawa
Affiliation:
Astrophysics Laboratory, Department of Physics, Faculty of Science, Chiba University, c/o Prof. Ryoji Matsumoto, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, Japan
Ryoji Matsumoto
Affiliation:
Department of Physics, Faculty of Science, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, Japan
Shigeki Miyaji
Affiliation:
Department of Physics, Faculty of Science, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, Japan
Tatsuo Yoshida
Affiliation:
Department of Physics, Faculty of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan

Extract

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In active massive star forming regions such as Orion and the Galactic center, the self-gravitational instability of a magnetized gaseous slab plays an important role as a trigger of star formation. In such high external pressure regions, the incompressible mode of self-gravitational instability (Elmegreen & Elmegreen 1978; Lubow & Pringle 1992) becomes dominant. Based on two-dimensional hydrodynamical simulations, Umekawa et al. (1999) proposed “Star formation by merging of the Jeans stable clumps” in a pressure bounded slab. In a magnetized slab confined by external pressure, Nagai et al. (1998) showed by linear analysis that the slab fragments to filaments parallel to the magnetic field lines. Here, we show by nonlinear three-dimensional MHD simulations that the filaments further fragment to Jeans stable clumps.

Type
Star Formation Regions and Outflow Processes in our Galaxy
Information
Symposium - International Astronomical Union , Volume 205: Galaxies and their Constituents at the Highest Angular Resolutions , 2001 , pp. 286 - 287
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Elmegreen, B. G., & Elmegreen, D. M. 1978, ApJ, 220, 1051.CrossRefGoogle Scholar
Lubow, S. H., & Pringle, J. E. 1993, MNRAS, 263, 701.Google Scholar
Meijerink, J. A., & van der Vorst, H. A. 1981, J. Comput. Phys., 44, 134.Google Scholar
Nagai, T., Inutsuka, S., & Miyama, S. M. 1998, ApJ, 506, 306.Google Scholar
Umekawa, M., Matsumoto, R., Miyaji, S., & Yoshida, T. 1999, PASJ, 51, 625.Google Scholar