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Theoretical efforts have struggled to produce slow rotation rates. In the absence of strong AM transport mechanisms within the massive star progenitor, NSs would invariably be born rotating near break-up. \citet{Heger_2005} and \citet{Suijs_2008} examined the effect of magnetic torques generated via the Tayler-Spruit (TS) dynamo \citep{spruit:02}, and found typical NS spin periods at birth (assuming AM conservation during core-collapse and the ensuing supernova) of several milliseconds. \citet{wheeler:14} implemented magnetic torques due to MRI and the TS dynamo, and were able to reach iron core rotation rates of $P_{c} \sim 500 \, {\rm s}$, corresponding to NS spin periods of $P \sim 25 \, {\rm ms}$. These efforts are promising, however, the operation of both mechanisms within stars has been debated \citep[e.g.]{Zahn_2007}, and theoretical uncertainties abound.  Recent asteroseismic advances have allowed for the measurement of core rotation rates in low mass red giant stars \citealt{beck:12,beck:14,mosser:12,deheuvels:12,deheuvels:14}. The measurements indicate that the cores of these stars rotate much slower than can be explained via hydrodynamic AM transport mechanisms or magnetic torques via the TS dynamo \citep{cantiello:14}. Although the cores rotate much faster than the surface (and and  one cannot assume nearly rigid rotation as suggested in \citet{spruit:98}, the slow core rotation rate suggests that cores of massive stars may rotate slower than expected. Internal gravity waves (IGW) constitute a powerful energy and AM transport mechanism. Several studies (\citealt{kumar:97,zahn:97,kumar:99,talon:02,talon:03,talon:05,talon:08,charbonnel:05,denissenkov:08,fullerwave:14}, hereafter F14) have found that convectively generated IGW can redistribute large quantities of AM within low-mass stars. IGW may partially account for the rigid rotation of the Sun's radiative interior and the slow rotation of red giant cores, although magnetic torques are also likely to be important (\citealt{denissenkov:08}, F14). IGW may also be important in more massive stars, and \cite{lee:14} found that convectively generated IGW in Be-type stars may instigate outbursts that expel mass into the decretion disk.