Conformal Yano-Killing tensors in einstein spacetimes

Self Cite

“…2 0 is a shift vector (B.4), g km ˜denotes an inverse of three-dimensional space metric and e mnp is a three-dimensional Levi-Civita tensor 5 .…”

Section: Discussionmentioning

confidence: 99%

Section: ( )mentioning

confidence: 99%

A geometric description of Maxwell field in a Kerr spacetime

Jezierski¹,

Smołka²

2016

Self Cite

“…Spin lowering the Weyl spinor using (35) gives the Maxwell field ψ ABCD κ CD , which has charges proportional to mass and dual mass, see also [33]. Letting M(C, κ) denote the corresponding closed complex two-form we have M(C, κ) = ψΨ 2 Z 1 .…”

Section: 2mentioning

confidence: 99%

“…For non-trivial κ AB , this restricts the spacetime to be of Petrov type D, N or O. For a given spacetime of type D in a principal tetrad (only 2 = 0), (33) becomes…”

Section: Conformal Killing-yano Tensors and Killing Spinorsmentioning

confidence: 99%

Charges for linearized gravity

Aksteiner¹,

Andersson²

2013

Abstract. Maxwell test fields as well as solutions of linearized gravity on the Kerr exterior admit non-radiating modes, i.e. non-trivial time-independent solutions. These are closely related to conserved charges. In this paper we discuss the non-radiating modes for linearized gravity, which may be seen to correspond to the Poincare Lie-algebra. The 2-dimensional isometry group of Kerr corresponds to a 2-parameter family of gauge-invariant non-radiating modes representing infinitesimal perturbations of mass and azimuthal angular momentum. We calculate the linearized mass charge in terms of linearized Newman-Penrose scalars.

“…to a Killing-Yano tensor, i.e. a skew 2-tensor K ab = K [ab] satisfying the Killing-Yano equation ∇ (a K b)c = 0, see [38,9,13,30] for further information. Let φ AB be the Maxwell spinor, i.e.…”

Section: Introductionmentioning

confidence: 99%

Linearized gravity and gauge conditions

Aksteiner

Andersson

2011

In this paper we consider the field equations for linearized gravity and other integer spin fields on the Kerr spacetime, and more generally on spacetimes of Petrov type D. We give a derivation, using the GHP formalism, of decoupled field equations for the linearized Weyl scalars for all spin weights and identify the gauge source functions occuring in these. For the spin weight 0 Weyl scalar, imposing a generalized harmonic coordinate gauge yields a generalization of the Regge-Wheeler equation. Specializing to the Schwarzschild case, we derive the gauge invariant Regge-Wheeler and Zerilli equation directly from the equation for the spin 0 scalar.