Angular momentum transport in magnetized stellar radiative zones. I - Numerical solutions to the core spin-up model problem

Details Angular momentum transport in magnetized stellar radiative zones. I - Numerical solutions to the core spin-up model problem Angular momentum transport in magnetized stellar radiative zones. I - Numerical solutions to the core spin-up model problem

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...387..639c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 387, March 10, 1992, p. 639-661.

Statistics

Computation

41

Angular Momentum, Magnetohydrodynamics, Momentum Transfer, Stellar Envelopes, Stellar Interiors, Stellar Magnetic Fields, Stellar Rotation, Computational Astrophysics, Magnetic Diffusion, Magnetic Field Configurations, Navier-Stokes Equation, Poloidal Flux, Reynolds Number

Scientific paper

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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