= Eddington-Sweet circulation
{c}
{title2=$t_{\rm ES}\sim t_{\rm KH}GM/(\Omega^2R^3)$}
The thermal imbalance of a slowly rotating radiative <star> can drive <stellar meridional circulation>. Its fractional centrifugal distortion is $\epsilon_\Omega\sim\Omega^2R^3/(GM)$, so balancing an order-$\epsilon_\Omega$ fraction of the <luminosity> by thermal advection estimates $t_{\rm ES}\sim t_{\rm KH}/\epsilon_\Omega$, where $t_{\rm KH}\sim GM^2/(RL)$. Stable composition gradients can further impede the circulation. This radiative thermal estimate is different from rapid torque-driven circulation in a convective envelope.
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