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The core rotation rates of massive stars have a substantial impact on thenature of core-collapse supernovae and their compact remnants. We demonstratethat internal gravity waves (IGW), excited via envelope convection during a redsupergiant phase or during vigorous late time burning phases, can have asignificant impact on the rotation rate of the pre-SN core. In typical ($10 \,M_\odot \lesssim M \lesssim 20 \, M_\odot$) supernova progenitors, IGW maysubstantially spin down the core, leading to iron core rotation periods $P_{\rmmin,Fe} \gtrsim 30 \, {\rm s}$. Angular momentum (AM) conservation during thesupernova would entail minimum NS rotation periods of $P_{\rm min,NS} \gtrsim 3\, {\rm ms}$. In most cases, the combined effects of magnetic torques and IGWAM transport likely lead to substantially longer rotation periods. However, thestochastic influx of AM delivered by IGW during shell burning phases inevitablyspin up a slowly rotating stellar core, leading to a maximum possible corerotation period. We estimate maximum iron core rotation periods of $P_{\rmmax,Fe} \lesssim 5 \times 10^3 \, {\rm s}$ in typical core-collapse supernovaprogenitors, and a corresponding spin period of $P_{\rm max, NS} \lesssim 500\, {\rm ms}$ for newborn neutron stars. This is comparable to the typical birthspin periods of most radio pulsars. Stochastic spin-up via IGW during shellO/Si burning may thus determine the initial rotation rate of most neutronstars. For a given progenitor, this theory predicts a Maxwellian distributionin pre-collapse core rotation frequency that is uncorrelated with the spin ofthe overlying envelope.

The spin rate of pre-collapse stellar cores: wave-driven angular momentum transport in massive stars