Cosmic string-seeded structure formation

We describe the results of high-resolution numerical simulations of string-induced structure formation using a cosmic string network with cold and hot dark matter backgrounds. The resulting linear power spectrum ${\cal P}(k)$ of density perturbations is calculated and compared with the linear power spectrum inferred from various galaxy surveys. We investigate the performance of cosmic string models in open universes and those with a non-zero cosmological constant. In particular, we show that for $\Gamma = \Omega h = 0.1--0.2$ both the mass fluctuation amplitude $\sigma_8$ at $8 h^{-1}$Mpc and the power spectrum shape of cosmic string-induced CDM fluctuations agree well with those inferred from observations. The HDM scenario with cosmic strings seems to require a strongly scale-dependent bias in order to be consistent with observations.