Kentaro Tanabe

Asymptotic flatness at null infinity in arbitrary dimensions

We define the asymptotic flatness and discuss asymptotic symmetry at null infinity in arbitrary dimensions using the Bondi coordinates. To define the asymptotic flatness, we solve the Einstein equations and look at the asymptotic behavior of gravitational fields. Then we show the asymptotic symmetry and the Bondi mass loss law with the well-defined definition.

On asymptotic structure at null infinity in five dimensions

We discuss the asymptotic structure of null infinity in five dimensional space-times. Since it is known that the conformal infinity is not useful for odd higher dimensions, we shall employ the coordinate based method such as the Bondi coordinate first introduced in four dimensions. Then we will define the null infinity and identify the asymptotic symmetry. We will also derive the Bondi mass expression and show its conservation law.

Asymptotic flatness at spatial infinity in higher dimensions

A definition of asymptotic flatness at spatial infinity in d dimensions (d≥4) is given using the conformal completion approach. Then we discuss asymptotic symmetry and conserved quantities. As in four dimensions, in d dimensions we should impose a condition at spatial infinity that the “magnetic” part of the d-dimensional Weyl tensor vanishes at a faster rate than the “electric” part does in order to realize the Poincare symmetry as asymptotic symmetry and construct the conserved angular momentum. However, we found that an additional condition should be imposed in d>4 dimensions.

Perturbative no-hair property of form fields for higher dimensional static black holes

In this paper we examine the static perturbation of

Static spacetimes with/without black holes in dynamical Chern-Simons gravity

p

Multipole moments for black objects in five dimensions

-form field strengths around higher dimensional Schwarzschild spacetimes. As a result, we can see that the static perturbations do not exist when

Universal quasinormal modes of black holes in the limit of large number of dimensions

p\ensuremath{\ge}3

Angular momentum at null infinity in five dimensions

. This result supports the no-hair properties of

Late-time symmetry near black hole horizons

p

Quasi-local characteristics of dynamical extreme black holes

-form fields. However, this does not exclude the presence of the black objects having nonspherical topology.