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\end{equation}  We calculate typical core convective velocities $v_{\rm con}$ using mixing length theory. In our stellar models, we evaluate equation \ref{eqn:beq} to find that core magnetic fields of $B \sim 3 \times 10^5 \, {\rm G}$ can be generated during the main sequence.  To extrapolate to field strengths plausibly obtained within the radiative cores of red giants, we assume that the magnetic flux (calculated via the methods above) within the core is conserved as it contracts. This is a good approximationas  for stable magnetic equilibriain the mass range  discussed here, here because  the timescale for the field to diffuse through the star (Ohmic (the Ohmic  timescale) is longer than the main sequence timescale. At each mass shell within a red giant, the field strength is then approximated by \begin{equation}  \label{eqn:BRG}  B_{\rm RG} = \bigg(\frac{r_{\rm MS}}{r_{\rm RG}}\bigg)^2 B_{\rm MS} \, ,