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\subsection{Stellar Models}  We have used the Modules for Experiments in Stellar Evolution (MESA, release #7385) code to evolve low-mass stars with initial mass in the range 1-2.5 $\mso$. Models have been evolved from the pre-main-sequence to the tip of the red giant branch \citep{Paxton_2010,Paxton_2013}. We chose a metallicity of $Z=0.02$ with a mixture taken from \citet{2005ASPC..336...25A}; the plasma opacity is determined using the OPAL opacity tables from \citet{Iglesias_1996}. Convective regions are calculated using the mixing-length theory (MLT) with $\alpha_{\rm MLT} = 2.0$. The boundaries of convective regions are determined using the Ledoux criterion. An exponentially decaying overshooting with $f_{\rm ov}= 0.018$ extends the mixing region beyond the convective boundaries \cite{2000A&A...360..952H}. We include in Section \ref{inlist} the inlist used for running the calculations.  To estimate the internal magnetic fields attainable in the cores of red giants, we first estimate the internal field strengths in main sequence stars. We do this in two ways. First, we extrapolate inward from the surface fields of $B \sim 1 \, {\rm kG}$ measured in magnetic Ap stars (***REF***), assuming the field is a pure dipole such that the field strength scales as $B \propto r^{-3}$. Since the radius of the convective core is typically $r_c \sim R/10$ for low mass main sequence stars, field strengths 2-3 orders in excess  of magnitude larger than the surface field strengths $B \gtrsim 10^{4} \, {\rm G}$  are easily  attainable near the core. 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 $B^2/(4 \pi) \sim \epsilon_{\rm con}/10$.