Results 131 to 140 of about 6,012 (165)
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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
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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
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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
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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.
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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 ...
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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 ...
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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.
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Distorted rotating black holes
Physics Letters A, 1984Abstract An axisymmetric stationary metric which describes rotating black holes distorted by surrounding matter is presented by means of the inverse scattering problem technique, and is written down explicitly in terms of the Legendre polynomials. A mass formula for the distorted holes is derived via the Komar integrals over the horizon.
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1992
Abstract In this chapter, we are going to make an effort to understand the Schwarz-schild vacuum solution. The solution (14.47) is exhibited in a particular coordinate system. In general, if we wish to write down a solution of the field equations, then we need to do so in some particular coordinate system.
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Abstract In this chapter, we are going to make an effort to understand the Schwarz-schild vacuum solution. The solution (14.47) is exhibited in a particular coordinate system. In general, if we wish to write down a solution of the field equations, then we need to do so in some particular coordinate system.
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Liquid Crystal Elastomer Twist Fibers toward Rotating Microengines
Advanced Materials, 2022Zhongqiang Yang
exaly