Non-gaussian Features of Linear Cosmic String Models

We investigate the non-gaussian properties of cosmic-string-seeded linear density perturbations with cold and hot dark matter backgrounds. These perturbations are computed using high-resolution numerical simulations with a dynamic range extending from before the radiation-matter transition through to deep into the matter era. We compute the one-point probability density function of the resulting density field, its skewness, kurtosis, and genus curves for different smoothing scales. A semi-analytic model is then invoked to provide a physical interpretation of our results. We conclude that on scales smaller than $1.5{(\Omega h^2)}^{-1}$Mpc, perturbations seeded by cosmic strings are very non-gaussian. These scales may still be in a linear or mildly non-linear regime in an open or $\Lambda$-universe with $\Gamma=\Omega h \lsim 0.2$