The present paper investigates the time evolution of the angular momentum and induced toroidal magnetic field distribution in an initially nonrotating radiative stellar envelope containing a large-scale poloidal magnetic field, following the impulsive spin-up of the underlying core. A large set of numerical calculations pertaining to monopolar, dipolar, and quadrupolar magnetic configurations, with and without density gradients across the envelope, as well as a set of solutions for which the poloidal field is only partially anchored on the core is presented. It is demonstrated that in moderate to high Reynolds-number systems, any global magnetic dissipation time scale constructed using length scales of order of the stellar radius greatly overestimates the true dissipation time scale of the toroidal magnetic component.
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Charbonneau et al. (1992) studied this question.