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\section{Stellar evolution calculations}  We use the Modules for Experiments in Stellar Evolution (MESA code) to evolve low-mass stars from the pre main sequence to the cooling WD sequence \citep{Paxton2011,Paxton2013}. This code includes the effects of the  centrifugal force on the stellar structure and structure,  chemical mixing and transport of angular momentum due to rotationally induced hydrodynamic instabilities \citep{Heger:2000}. The mixing of 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. %To account for the changes in the distribution of internal angular momentum during the long timescales of stellar evolution, modern stellar evolution %codes include a treatment of angular momentum and chemical mixing due to rotational instabilities and magnetic torques. In fact it has been shown that %it is still possible to treat this problem in 1D if the star is well mixed on horizontal surfaces. The existence of strong anisotropic turbulence in %stars is expected to enforce a constant composition and angular velocity on isobaric surfaces, the so-called ``shellular'' approximation %\citep{Zahn:1992}. The impact of the centrifugal term can be easily included in the equation of stellar structure \citep{Endal:1976}, while the effect %of transport of angular momentum and chemicals in the radial direction requires a simplified treatment of the rotational instabilities and circulations %expected to arise in a rotating star \citep[See e.g.][]{Heger:2000,Maeder:2000}. Dynamo action seems to be ubiquitous in astrophysical plasma, and   %the presence of magnetic fields can lead to efficient transport of angular momentum through magnetic torques. In radiative zones the presence of %magnetic fields has been discussed to explain the final rotation rate of compact remnants \citep[both white dwarfs and neutron stars,][]%{Heger_Langer_Woosley_2000,larends_Yoon_Heger_Herwig_2008}.