Late time tails of the massive vector field in a black hole background
| dc.creator | Konoplya, R. A. | |
| dc.creator | Molina, C. | |
| dc.creator | Zhidenko, A. | |
| dc.date | 2006-02-13 | |
| dc.date | 2007-02-06 | |
| dc.date.accessioned | 2026-07-07T10:28:15Z | |
| dc.date.available | 2026-07-07T10:28:15Z | |
| dc.description | We investigate the late-time behavior of the massive vector field in the background of the Schwarzschild and Schwarzschild-de Sitter black holes. For Schwarzschild black hole, at intermediately late times the massive vector field is represented by three functions with different decay law $Ψ_{0} \sim t^{-(\ell + 3/2)} \sin{m t}$, $Ψ_{1} \sim t^{-(\ell + 5/2)} \sin{m t}$, $Ψ_{2} \sim t^{-(\ell + 1/2)} \sin{m t}$, while at asymptotically late times the decay law $Ψ\sim t^{-5/6} \sin{(m t)}$ is universal, and does not depend on the multipole number $\ell$. Together with previous study of massive scalar and Dirac fields where the same asymptotically late-time decay law was found, it means, that the asymptotically late-time decay law $\sim t^{-5/6} \sin{(m t)}$ \emph{does not depend} also \emph{on the spin} of the field under consideration. For Schwarzschild-de Sitter black holes it is observed two different regimes in the late-time decay of perturbations: non-oscillatory exponential damping for small values of $m$ and oscillatory quasinormal mode decay for high enough $m$. Numerical and analytical results are found for these quasinormal frequencies. | |
| dc.description | one author and new material are added | |
| dc.identifier | https://arxiv.org/abs/gr-qc/0602047 | |
| dc.identifier | http://arxiv.org/abs/gr-qc/0602047 | |
| dc.identifier | Phys.Rev.D75:084004,2007 | |
| dc.identifier | doi:10.1103/PhysRevD.75.084004 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/177382 | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.title | Late time tails of the massive vector field in a black hole background | |
| dc.type | text |