Evolution of magnetized, rotating, isothermal clouds

Details Evolution of magnetized, rotating, isothermal clouds Evolution of magnetized, rotating, isothermal clouds

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nascp3084..255t&link_type=abstract

In NASA, Ames Research Center, The Interstellar Medium in External Galaxies: Summaries of Contributed Papers p 255-257 (SEE N91-

Physics

Galactic Rotation, Magnetic Clouds, Magnetic Fields, Magnetic Flux, Molecular Clouds, Rotation, Star Formation, Zeeman Effect, Angular Momentum, Background Radiation, Collapse, Near Infrared Radiation, Shapes

Scientific paper

Molecular cloud cores, in which star formation process now proceeds, are often found with elongated shape. This suggests that the core collapsed preferentially along the direction parallel to the global magnetic field and/or parallel to the cloud's initial angular momentum. Actually the magnetic field strength in the cloud has been measured recently with the Zeeman splitting (Goodman et al. 1989). The authors indicate the magnetic field of 10 to 30 mu G exists in the cloud. Further, the observation of polarization in the near IR from background stars shows that the magnetic field runs perpendicularly to the major axis of the cloud (Tamura et al. 1987). As for the angular momentum, the rotation rate of 0.2 to 6 kms s-1 pc-1 is reported (Goldsmith and Arquilla 1984) in 16 dark cloud regions. If the cloud collapses from the diffuse cloud with density n approx. 1 cm -3 with strictly conserving the angular momentum which was shared from the galactic rotation, the rotation rate of the cloud will be x megaj = const approx. 3(n/1000 cm exp -3) exp 2/3 km s-1 pc -1 (Mouschovias 1987). The evolution of the rotating magnetized cloud is discussed here.

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