Molecular Cloud Collapse

Details Molecular Cloud Collapse Molecular Cloud Collapse

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ap%26ss.292..361a&link_type=abstract

Astrophysics and Space Science, v. 292, Issue 1, p. 361-364 (2004).

Astronomy and Astrophysics

Astrophysics

Ism: Clouds, Magnetohydrodynamics, Star Formation

Scientific paper

Theoretical models of star formation from the collapse of molecular cloud cores have been evolving in complexity for many years. This work describes the evolution of models from the nonrotating, nonmagnetized singular isothermal sphere to rotating, magnetized singular isothermal toroids. Four members of the same family are studied the four combinations of nonrotation/rotation and nonmagnetization/magnetization. It is found that although rotation alone can hinder collapse to a pointmass, addition of braking from a magnetic field can transport away much of the angular momentum upward in a low-velocity outflow during the collapse phase. For all magnetized cases, accretion proceeds at a constant rate similar to that of the isothermal sphere.

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