Cosmic-String–Seeded Structure Formation

We describe the results of high-resolution numerical simulations of string-induced structure formation in open universes and those with a nonzero cosmological constant. For models with $\Gamma =\Omega h=0.1–0.2$ and a cold dark matter background, we show that the linear density fluctuation power spectrum has both an amplitude at ${8h}^{-1\mathrm{}}\mathrm{Mpc}$, ${\sigma }_8$, and an overall shape which are consistent within uncertainties with those currently inferred from galaxy surveys. The cosmic string scenario with hot dark matter requires a strongly scale-dependent bias in order to agree with observations.