Improving the Lagrangian perturbative solution for cosmic fluid: Applying Shanks transformation
| dc.creator | Tatekawa, Takayuki | |
| dc.date | 2006-05-10 | |
| dc.date | 2007-02-25 | |
| dc.date.accessioned | 2026-07-07T10:23:05Z | |
| dc.date.available | 2026-07-07T10:23:05Z | |
| dc.description | We study the behavior of Lagrangian perturbative solutions. For a spherical void model, the higher order the Lagrangian perturbation we consider, the worse the approximation becomes in late-time evolution. In particular, if we stop to improve until an even order is reached, the perturbative solution describes the contraction of the void. To solve this problem, we consider improving the perturbative solution using Shanks transformation, which accelerates the convergence of the sequence. After the transformation, we find that the accuracy of higher-order perturbation is recovered and the perturbative solution is refined well. Then we show that this improvement method can apply for a $Λ$CDM model and improved the power spectrum of the density field. | |
| dc.description | 17 pages, 7 figures; accepted for publication in Phys.Rev.D; v2: Evolution of power spectrum in LCDM model is added; v3: References are corrected | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0605250 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0605250 | |
| dc.identifier | Phys.Rev.D75:044028,2007 | |
| dc.identifier | doi:10.1103/PhysRevD.75.044028 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/175702 | |
| dc.subject | Astrophysics | |
| dc.title | Improving the Lagrangian perturbative solution for cosmic fluid: Applying Shanks transformation | |
| dc.type | text |