deletions | additions       diff --git a/Stellar evolution calculations.tex b/Stellar evolution calculations.tex  index 65784bc..497c366 100644  --- a/Stellar evolution calculations.tex  +++ b/Stellar evolution calculations.tex 
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%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}.   We chose an initial metallicity of $Z=0.02$ with a mixture taken from \citet{Asplund:2005}. We adopt the OPAL opacity tables \citep{Iglesias:1996} accounting for the carbon- and oxygen- enhanced opacities during helium burning \citep[Type 2 OPAL,][]{Iglesias:1993}.  Solid body rotation is set at the zero age main sequence (ZAMS). Convective regions are calculated using the mixing length theory (MLT) in the \citet{Henyey:1965} formulation with $\alphaMLT=1.6$. Transport of angular momentum in convective regions is accounted for using the resulting MLT diffusion coefficient (turbulent diffusivity), which is generally very high and leads to rigid rotation in convective zones. While this seems to be the case in the Sun, another possible treatment of rotating convective zones is adopting a constant specific angular momentum \citep[See e.g.][]{Kawaler:2005}. We rana few  calculations with this assumption and found that it does not affect the results conclusions  in this paper. The boundaries of convective regions are determined using the Ledoux criterion. Semiconvection is accounted for in the Langer prescription \citep{Langer:1983,Langer:1985} with an efficiency $\alphasc=$0.003. A step function overshooting extends for 0.2 pressure scale heights   the mixing region beyond the convective boundary during core H-burning. %MC: Check if it's also extending core He-burning  We also account for gravitational settling and chemical diffusion \citep{Paxton2011}.