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Our second technique is predicated on the existence of a magnetic field generated by a dynamo in the convective core of the main sequence star. We calculate the mixing-length theory convective velocities from our stellar models to estimate the kinetic energy density $\epsilon_{\rm con} = \rho v_{\rm con}^2$ available to drive a dynamo. We then assume the magnetic field attains a sub-equiparition field strength of $B^2/(8 \pi) \sim \epsilon_{\rm con}/10$. Once again, we find that field strengths in excess of $10^4 \,{\rm G}$ can easily be obtained just outside of the convective core of an $M \sim 1.6 M_\odot$ star.  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 approximation as for stable magnetic equilibria and the mass range discussed here, the timescale for the field to diffuse through the star (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} \, ,