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We propose a simple model to explain the velocity of young neutron stars. Weattempt to confirm a relationship between the amount of mass ejected in theformation of the neutron star and the `kick' velocity imparted to the compactremnant resulting from the process. We assume the velocity is given by $v_{\rmkick}=\alpha\,(M_{\rm ejecta} / M_{\rm remnant}) + \beta\,$. To test thissimple relationship we use the BPASS (Binary Population and Spectral Synthesis)code to create stellar population models from both single and binary starevolutionary pathways. We then use our Remnant Ejecta and Progenitor ExplosionRelationship (REAPER) code to apply different $\alpha$ and $\beta$ values andthree different `kick' orientations then record the resulting velocityprobability distributions.  We find that while a single star population provides a poor fit to theobservational data, the binary population provides an excellent fit. Values of$\alpha=70\, {\rm km\,s^{-1}}$ and $\beta=110\,{\rm km\,s^{-1}}$ reproduce the\cite{RN165} observed 2-dimensional velocities and $\alpha=70\, {\rmkm\,s^{-1}}$ and $\beta=120\,{\rm km\,s^{-1}}$ reproduce their inferred3-dimensional velocity distribution for nearby single neutron stars with agesless than 3 Myrs. After testing isotropic, spin-axis aligned and orthogonal tospin-axis `kick' orientations, we find no statistical preference for a `kick'orientation. While ejecta mass cannot be the only factor that determines thevelocity of supernovae compact remnants, we suggest it is a significantcontributor and that the ejecta based `kick' should replace theMaxwell-Boltzmann velocity distribution currently used in many populationsynthesis codes.

Neutron Star Kicks and their Relationship to Supernovae Ejecta Mass