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Flexoelectric domain walls enable charge separation and transport in cubic perovskites. [PDF]
Nat CommunRak D +5 more
europepmc +1 more source
, 2019 For this last lecture, we will focus on particular properties of astrophysically realistic 4d black holes, which are rotating and uncharged. We will concentrate on the stationary Kerr black hole solution which is the final state of collapse of matter.
Şahin Polat, Damla
core +3 more sources
Area spectrum of slowly rotating black holes
Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics, 2010 We investigate the area spectrum for rotating black holes which are Kerr and BTZ black holes. For slowly rotating black holes, we use the Maggiore's idea combined with Kunstatter's method to derive their area spectra, which are equally ...
Yun Soo Myung
exaly +2 more sources
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2022
Abstract Chapter 20, the final chapter in Part D, looks at the Kerr solution, which describes a rotating black hole. It turns out to be a rather long process to solve Einstein’s vacuum equations directly for the Kerr solution, so the chapter instead describes a ‘trick’ used by Newman and Janis for obtaining the Kerr solution from the ...
Ray d’Inverno, James Vickers
openaire +1 more source
Abstract Chapter 20, the final chapter in Part D, looks at the Kerr solution, which describes a rotating black hole. It turns out to be a rather long process to solve Einstein’s vacuum equations directly for the Kerr solution, so the chapter instead describes a ‘trick’ used by Newman and Janis for obtaining the Kerr solution from the ...
Ray d’Inverno, James Vickers
openaire +1 more source
Rotating Black Holes and Black Hole Mechanics
2019In this section, we consider rotating black holes as well as black hole mechanics and start exploring its similarities with thermodynamics.
Dieter Lüst, Ward Vleeshouwers
openaire +1 more source
1998
In the preceding chapters we have demonstrated that the gravitational collapse of a spherical nonrotating mass produces a spherically symmetric black hole when the. radius of the body becomes less than the gravitational radius. In Section 3.4 we have shown that after a black hole has been formed in the collapse of a body slightly deviating from ...
Valeri P. Frolov, Igor D. Novikov
openaire +1 more source
In the preceding chapters we have demonstrated that the gravitational collapse of a spherical nonrotating mass produces a spherically symmetric black hole when the. radius of the body becomes less than the gravitational radius. In Section 3.4 we have shown that after a black hole has been formed in the collapse of a body slightly deviating from ...
Valeri P. Frolov, Igor D. Novikov
openaire +1 more source
Journal of Astrophysics and Astronomy, 1999
In this article, we first consider briefly the basic properties of the non-rotating Schwarzschild black hole and the rotating Kerr black hole Rotational effects are then described in static and stationary spacetimes with arial symmetry by studying inertial forces, gyroscopic precession and gravi-electromagnetism.
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In this article, we first consider briefly the basic properties of the non-rotating Schwarzschild black hole and the rotating Kerr black hole Rotational effects are then described in static and stationary spacetimes with arial symmetry by studying inertial forces, gyroscopic precession and gravi-electromagnetism.
openaire +1 more source
1984
All stars rotate more or less rapidly. When a horizon is formed during gravitational collapse, a Schwarzschild black hole is thus never produced. One expects, however, that the horizon will quickly settle down to a stationary state as a result of the emission of gravitational waves.
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All stars rotate more or less rapidly. When a horizon is formed during gravitational collapse, a Schwarzschild black hole is thus never produced. One expects, however, that the horizon will quickly settle down to a stationary state as a result of the emission of gravitational waves.
openaire +1 more source
1992
Abstract In this chapter, we shall investigate the Kerr solution which describes rotating black holes. It turns out to be a rather long process to solve Einstein’s vacuum equations directly for the Kerr solution. We shall, instead, describe a ‘trick’ of Newman and Janis for obtaining the Kerr solution from the Schwarzschild solution ...
openaire +1 more source
Abstract In this chapter, we shall investigate the Kerr solution which describes rotating black holes. It turns out to be a rather long process to solve Einstein’s vacuum equations directly for the Kerr solution. We shall, instead, describe a ‘trick’ of Newman and Janis for obtaining the Kerr solution from the Schwarzschild solution ...
openaire +1 more source