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Matteo Cantiello deleted file Angular Momentum Transport.tex
almost 11 years ago
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\subsection{Angular Momentum Transport}
Different processes that are believed to be responsible for transport of angular momentum in stellar interiors enter a diffusion equation of the kind:
\begin{equation}
\dxdycz{\omega}{t}{m}=\frac{1}{i}\,\dxdycz{}{m}{t}\,
\SBrak{(4\pi r^2 \rho)^2 \, i\nu \,\dxdycz{\omega}{m}{t}}-\frac{2\omega}{r}\,\dxdycz{r}{t}{m}
\, \Brak{\frac{1}{2}\frac{\dif\ln i}{\dif\ln r}} \,
\end{equation}\label{e.jdiff}
where $i$ is the specific moment of inertia of a shell at mass
coordinate $m$, and $\nu$ is the turbulent viscosity
determined as the sum of the diffusion coefficients for convection, double diffusion,
overshooting, rotationally-induced instabilities and Spruit-Tayler (ST) magnetic fields. The diffusive transport is carefully implemented to
accurately conserve angular momentum.
