The images above show the numerical values describing the initial polytropic equation of state and the characteristic strength of the initial magnetic field. These cases are characterized by an accumulation of the majority of the mass at the center, following magnetic braking and viscous damping of differential rotation. The outermost mass shells expand out and form an ambient disk surrounding the star and a wind.
The colorbar shown above is used for all but one of the n=3 cases (the exception is the zoomed out view for the nonviscous simulation). The densities have been normalized to the initial central density.
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