Angular momentum transport in massive stars and natal neutron star rotation rates

Understand

The internal rotational dynamics of massive stars are poorly understood.

• If angular momentum (AM) transport between the core and the envelope is inefficient, the large core AM upon core-collapse will produce rapidly rotating neutron stars (NSs).
• However, observations of low-mass stars suggest an efficient AM transport mechanism is at work, which could drastically reduce NS spin rates.
• Here we study the effects of the baroclinic instability and the magnetic Tayler instability in differentially rotating radiative zones.