deletions | additions       diff --git a/Introduction.tex b/Introduction.tex  index b156147..83fc0c0 100644  --- a/Introduction.tex  +++ b/Introduction.tex 
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%Therefore an important test of   %While their pre-main sequence evolution is complex, a common assumption is that these stars reach a state of quasi-solid rotation when they start burning hydrogen at the zero %age main sequence. From there on the evolution has to account for the loss and the internal redistribution of angular momentum through d. Therefore stellar evolution models need %to include the important physical processes that dominate the angular momentum transport in the stellar interiors. Here we discuss how state-of-the-art stellar evolution %calculations of low-mass stars perform compared to some observational tests of their rotational properties.  Low-mass %Low-mass  stars evolve past the main sequence toward their red giant stage. In this phase the star experience \citet{lo_Langer_Pols_Brott_Yoon_2009}