## 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.

## 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.
doi:10.1007/BF00763405.

Demianski, M.
1976.
"Stationary axially symmetric perturbations of a rotating black hole. [Space-time perturbation, Newman-Penrose formalism]."
United Kingdom.
doi:10.1007/BF00763405.
https://www.osti.gov/servlets/purl/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 = {Gen. Relativ. Gravitation; (United Kingdom)}

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 = {Gen. Relativ. Gravitation; (United Kingdom)}

volume = {7:7}

journal type = {AC}

place = {United Kingdom}

year = {1976}

month = {Jul}

}