= Gyroscopic pumping in a star
{title2=$\rho\mathbf v_m\cdot\nabla(\varpi^2\Omega)=-\nabla\cdot\mathbf F_J$}
In a steady axisymmetric <star>, a torque due to <Reynolds stress>, <Maxwell stress tensor> or <viscosity> must balance advection of <specific angular momentum> by <stellar meridional circulation>. Writing the nonadvective <angular momentum transport> flux as $\mathbf F_J$ gives the displayed balance. Thus stresses that maintain <differential rotation> also drive a meridional response. The <stellar thermal-wind balance> supplies a separate leading force constraint, not a replacement for this torque equation.
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