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\section{Stellar evolution calculations}  We use the Modules for Experiments in Stellar Evolution (MESA) to evolve low-mass stars from the pre main sequence to the cooling WD sequence \citep{Paxton2011,Paxton2013}. This code includes the centrifugal force on the stellar structure and chemical mixing and transport of angular momentum due to rotationally induced hydrodynamic instabilities \citep{Heger:2000}. The mixing of chemicals and angular momentum due to dynamo-generated magnetic fields in radiation zones is also included \citep{Spruit:2002,Petrovic:2005,Heger:2005}. See \citet{Paxton2013} for the details of the implementation of rotation and magnetic fields in MESA.  We adopt an initial metallicity of $Z=0.02$ with a mixture taken from \citet{Asplund:2005}. Convective regions are calculated using the Mixing Length Theory in the \citet{Henyey:1965} formulation with $\alphaMLT=1.6$.  % mixing_length_alpha = 1.6   % use_Henyey_MLT = .true.   % use_Ledoux_criterion = .true.   % alpha_semiconvection = 1d-3   % semiconvection_option = 'Langer_85'   % thermo_haline_coeff = 0.0   % ! Set to 0.335 over h-burn, off for all else   % overshoot_f_above_burn_h = 0.2 ! Brott et al. 2011   % overshoot_f0_above_burn_h = 0.   % overshoot_step_fraction = 1. ! Step function     % !---------------------------------------- ELEMENT DIFFUSION     % do_element_diffusion = .true.