“Kerr-Schild perturbations”的意思、由来-开放百科全书

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Kerr-Schild perturbations

释义

Form
Applications
References

Kerr-Schild perturbations are a special type of perturbation to a spacetime metric which only appear linearly in the Einstein field equations which describe General Relativity. They were found by Roy Kerr and Alfred Schild in 1965.^[1]

Form

A generalised Kerr-Schild perturbation has the form , where is a scalar and is a null vector with respect to the background spacetime.^[2] It can be shown that any perturbation of this form will only appear quadratically in the Einstein equations, and only linearly if the condition , where is a scalar, is imposed. This condition is equivalent to requiring that the orbits of are geodesics.^[2]

Applications

While the form of the perturbation may appear very restrictive, there are several black hole metrics which can be written in Kerr-Schild form, such as Schwarzschild (stationary black hole), Kerr (rotating), Reissner–Nordström (charged) and Kerr-Newman (both charged and rotating).^[2]^[3]

References

1. ^{{cite web|url=https://link.springer.com/article/10.1007/s10714-009-0857-z|title=Republication of: A new class of vacuum solutions of the Einstein field equations|website=SpringerLink|accessdate=2019-03-26}}
2. ^¹²{{cite web|url=https://journals.aps.org/prd/abstract/10.1103/PhysRevD.94.084009|title=Phys. Rev. D 94, 084009 (2016) - Generating exact solutions to Einstein's equation using linearized approximations|website=journals.aps.org|accessdate=2019-03-26}}
3. ^{{cite web|url=https://iopscience.iop.org/article/10.1088/0264-9381/11/6/010/meta|title=Distributional energy--momentum tensor of the Kerr--Newman spacetime family|website=IOPscience|accessdate=2019-03-26}}

1 : General relativity

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