Rotating normal and phantom Einstein-Maxwell-dilaton black holes:
  Geodesics analysis

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Abstract

Depending on five parameters, rotating counterparts of Einstein-Maxwell-dilaton black holes are derived. We discuss their physical and geometric properties and investigate their null and time-like geodesics including circular orbits. The Lense-Thirring effect is considered.

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Most cited references 10

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Radiation from relativistic particles in nongeodesic motion in a strong gravitational field

A. Aliev, D. Galtsov (1981)

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Phantom Black Holes in Einstein-Maxwell-Dilaton Theory

Manuel Eleuterio Rodrigues, Júlio C. Fabris, Gérard Clément (2009)

We obtain the general static, spherically symmetric solution for the Einstein-Maxwell-dilaton system in four dimensions with a phantom coupling for the dilaton and/or the Maxwell field. This leads to new classes of black hole solutions, with single or multiple horizons. Using the geodesic equations, we analyse the corresponding Penrose diagrams revealing, in some cases, new causal structures.

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An explanation of the Newman-Janis Algorithm

S. Szekeres, Samuel Drake (1998)

After the original discovery of the Kerr metric, Newman and Janis showed that this solution could be ``derived'' by making an elementary complex transformation to the Schwarzschild solution. The same method was then used to obtain a new stationary axisymmetric solution to Einstein's field equations now known as the Kerr-newman metric, representing a rotating massive charged black hole. However no clear reason has ever been given as to why the Newman-Janis algorithm works, many physicist considering it to be an ad hoc procedure or ``fluke'' and not worthy of further investigation. Contrary to this belief this paper shows why the Newman-Janis algorithm is successful in obtaining the Kerr-Newman metric by removing some of the ambiguities present in the original derivation. Finally we show that the only perfect fluid generated by the Newman-Janis algorithm is the (vacuum) Kerr metric and that the only Petrov typed D solution to the Einstein-Maxwell equations is the Kerr-Newman metric.