deletions | additions       diff --git a/sectionIntroduction_.tex b/sectionIntroduction_.tex  index 1818580..359e713 100644  --- a/sectionIntroduction_.tex  +++ b/sectionIntroduction_.tex 
...
In this paper, we examine AM transport due to convectively excited IGW within massive stars, focusing primarily on AM transport due to late burning stages (He, C, O, and Si burning). We find that IGW are generally capable of redistributing large amounts of AM before CC despite the short stellar evolution time scales. IGW emitted from convective shells propagate into the radiative core and can substantially slow its rotation. We also show that stochastic influxes of AM via IGW set a minimum core rotation rate which may account for a large population of slowly rotating ($P \gtrsim 100 \,{\rm ms}$) NSs, if AM is mostly conserved during a supernova.   Our paper is organized as follows...Section \ref{intro} is the introduction.