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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.