Cosmic-String-Seeded Structure Formation
| dc.creator | Avelino, P. P. | |
| dc.creator | Shellard, E. P. S. | |
| dc.creator | Wu, J. H. P. | |
| dc.creator | Allen, B. | |
| dc.date | 1997-11-30 | |
| dc.date | 1998-09-03 | |
| dc.date.accessioned | 2026-07-07T11:34:07Z | |
| dc.date.available | 2026-07-07T11:34:07Z | |
| dc.description | We describe the results of high-resolution numerical simulations of string-induced structure formation in open universes and those with a non-zero cosmological constant. For models with $Γ= Ωh = 0.1 - 0.2$ and a cold dark matter background, we show that the linear density fluctuation power spectrum has both an amplitude at $8 h^{-1} Mpc, σ_8$, 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. | |
| dc.description | 5 pages, 3 figures; to appear in Phys. Rev. Lett. (Sept. 1998). With a cosmological constant included in the evolution equation (1), and simulations carried out accordingly. This verifies the accuracy of the extrapolation scheme for $Λ$-models taken previously. Also corrected for a minor error in the standard normalization of wavenumbers $k$, resulting from using an incorrect figure for the time $t_{eq}$ of the equal matter-radiation transition given in the Kolb and Turner textbook "The Early Universe". Main conclusions remain unchanged | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9712008 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9712008 | |
| dc.identifier | Phys.Rev.Lett.81:2008-2011,1998 | |
| dc.identifier | doi:10.1103/PhysRevLett.81.2008 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/198134 | |
| dc.subject | Astrophysics | |
| dc.title | Cosmic-String-Seeded Structure Formation | |
| dc.type | text |