Abstract
A stationary axially symmetric perturbation of a rotating black hole due to a distribution of test matter is investigated. The Newman-Penrose spin coefficient formalism is used to derive a general set of equations describing the perturbed space-time. In a linear approximation it is shown that the mass and angular momentum of a rotating black hole is not affected by the perturbation. The metric perturbations near the horizon are given. It is concluded that given a perturbing test fluid distribution, one can always find a corresponding metric perturbation such that the mass and angular momentum of the black hole are not changed. It was also noticed that when a tends to M, those perturbed spin coefficients and components of the Weyl tensor which determine the intrinsic properties of the incoming null cone near the horizon grow indefinitely.
Demianski, M
[1]
- California Inst. of Tech., Pasadena (USA)
Citation Formats
Demianski, M.
Stationary axially symmetric perturbations of a rotating black hole. [Space-time perturbation, Newman-Penrose formalism].
United Kingdom: N. p.,
1976.
Web.
doi:10.1007/BF00763405.
Demianski, M.
Stationary axially symmetric perturbations of a rotating black hole. [Space-time perturbation, Newman-Penrose formalism].
United Kingdom.
https://doi.org/10.1007/BF00763405
Demianski, M.
1976.
"Stationary axially symmetric perturbations of a rotating black hole. [Space-time perturbation, Newman-Penrose formalism]."
United Kingdom.
https://doi.org/10.1007/BF00763405.
@misc{etde_7313278,
title = {Stationary axially symmetric perturbations of a rotating black hole. [Space-time perturbation, Newman-Penrose formalism]}
author = {Demianski, M}
abstractNote = {A stationary axially symmetric perturbation of a rotating black hole due to a distribution of test matter is investigated. The Newman-Penrose spin coefficient formalism is used to derive a general set of equations describing the perturbed space-time. In a linear approximation it is shown that the mass and angular momentum of a rotating black hole is not affected by the perturbation. The metric perturbations near the horizon are given. It is concluded that given a perturbing test fluid distribution, one can always find a corresponding metric perturbation such that the mass and angular momentum of the black hole are not changed. It was also noticed that when a tends to M, those perturbed spin coefficients and components of the Weyl tensor which determine the intrinsic properties of the incoming null cone near the horizon grow indefinitely.}
doi = {10.1007/BF00763405}
journal = []
volume = {7:7}
journal type = {AC}
place = {United Kingdom}
year = {1976}
month = {Jul}
}
title = {Stationary axially symmetric perturbations of a rotating black hole. [Space-time perturbation, Newman-Penrose formalism]}
author = {Demianski, M}
abstractNote = {A stationary axially symmetric perturbation of a rotating black hole due to a distribution of test matter is investigated. The Newman-Penrose spin coefficient formalism is used to derive a general set of equations describing the perturbed space-time. In a linear approximation it is shown that the mass and angular momentum of a rotating black hole is not affected by the perturbation. The metric perturbations near the horizon are given. It is concluded that given a perturbing test fluid distribution, one can always find a corresponding metric perturbation such that the mass and angular momentum of the black hole are not changed. It was also noticed that when a tends to M, those perturbed spin coefficients and components of the Weyl tensor which determine the intrinsic properties of the incoming null cone near the horizon grow indefinitely.}
doi = {10.1007/BF00763405}
journal = []
volume = {7:7}
journal type = {AC}
place = {United Kingdom}
year = {1976}
month = {Jul}
}