Perturbations of slowly rotating black holes: massive vector fields in the Kerr metric
作者： Paolo Pani , Vitor Cardoso , Leonardo Gualtieri , Emanuele Berti , Akihiro Ishibashi
DOI: 10.1103/PHYSREVD.86.104017
关键词:
摘要: We discuss a general method to study linear perturbations of slowly rotating black holes which is valid for any perturbation field, and particularly advantageous when the field equations are not separable. As an illustration we investigate massive vector (Proca) in Kerr metric, do appear be separable standard Teukolsky formalism. Working perturbative scheme, two important effects induced by rotation: Zeeman-like shift nonaxisymmetric quasinormal modes bound states with different azimuthal number $m$, coupling between axial polar multipolar index $\ensuremath{\ell}$. explicitly compute up second order rotation, but principle can extended order. at first rotation show that Proca computed solving decoupled sets equations, derive single master equation describing spin $s=0$ $s=\ifmmode\pm\else\textpm\fi{}1$. By extending calculation superradiant regime self-consistent way. For time fields around exhibit instability, significantly stronger than scalar fields. Because this astrophysical observations spinning provide tightest upper limit on mass photon: ${m}_{\ensuremath{\gamma}}\ensuremath{\lesssim}4\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}20}\text{ }\text{ }\mathrm{eV}$ under our most conservative assumptions. Spin measurements largest could reduce ${m}_{\ensuremath{\gamma}}\ensuremath{\lesssim}{10}^{\ensuremath{-}22}\text{ or lower.
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