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Using twenty long-term 3D core-collapse supernova simulations, we find thatlower compactness progenitors that explode quasi-spherically due to the shortdelay to explosion experience smaller neutron star recoil kicks in the$\sim$100$-$200 km s$^{-1}$ range, while higher compactness progenitors thatexplode later and more aspherically leave neutron stars with kicks in the$\sim$300$-$1000 km s$^{-1}$ range. In addition, we find that these two classesare correlated with the gravitational mass of the neutron star. Thiscorrelation suggests that the survival of binary neutron star systems may inpart be due to their lower kick speeds. We also find a correlation of the kickwith both the mass dipole of the ejecta and the explosion energy. Furthermore,one channel of black hole birth leaves masses of $\sim$10 $M_{\odot}$, is notaccompanied by a neutrino-driven explosion, and experiences small kicks. Asecond is through a vigorous explosion that leaves behind a black hole with amass of $\sim$3.0 $M_{\odot}$ kicked to high speeds. We find that the inducedspins of nascent neutron stars range from seconds to $\sim$10 milliseconds andthat a spin/kick correlation for pulsars emerges naturally. We suggest that ifan initial spin biases the explosion direction, a spin/kick correlation is acommon byproduct of the neutrino mechanism of core-collapse supernovae.Finally, the induced spin in explosive black hole formation is likely large andin the collapsar range. This new 3D model suite provides a greatly expandedperspective and appears to explain some observed pulsar properties by default.

A Comprehensive Theory for Neutron Star and Black Hole Kicks and Induced Spins