Painlevé–Gullstrand coordinates for Schwarzschild–de Sitter spacetime

Volovik, G. E.

doi:10.1016/j.aop.2023.169219

Cited by 5 publications

(1 citation statement)

References 52 publications

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“…Hence those hypersurfaces are nice slices in the modest sense. Recently, research concerning PG time slices has given alternative viewpoints for studying cosmology and embedding a black hole into an expanding Universe [31,32]. Nevertheless, we are inspired by the wide-range usage of nice slices to propose the trick for calculating surface gravities.…”

Section: Introductionmentioning

confidence: 99%

A trick for calculating surface gravities of Killing horizons

Yang

2024

Class. Quantum Grav.

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Section: Introductionmentioning

confidence: 99%

A trick for calculating surface gravities of Killing horizons

Yang

2024

Class. Quantum Grav.

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Tetrad formalism in the solution of spherically symmetric spacetime in general relativity

Wulandari,

Subagyo,

Rahmani

2024

J. Phys.: Conf. Ser.

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Spherically symmetric solutions in general relativity are the most fundamental solutions to the Einstein field equation. The first exact solution of the Einstein field equation is the spherically symmetric solution given by the Schwarzschild metric, as easily found in any standard textbook on general relativity. The FLRW (Friedmann-Lemaitre-Robertson-Walkers) metric is another spherically symmetric solution of Einstein’s equation describing the standard model in Cosmology. The standard approach to solving Einstein’s equations is by considering the metric. However, we can also adopt a tetrad-based method or tetrad formalism. We review these two solutions by the tetrad formalism as an alternative approach. In addition, we give some more cases, including the cosmological constant and the Taub-NUT metric.

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On the Global Temperature of the Schwarzschild–de Sitter Spacetime

Volovik

2023

Jetp Lett.

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It is shown that the Schwarzschild–de Sitter spacetime has the universal temperature. This temperature describes the thermal processes of decay of the composite particles and the other processes, which are energetically forbidden in the Minkowski spacetime, but are allowed in the de Sitter and in Schwarzschild–de Sitter backgrounds. In particular, this temperature describes the probability of ionization of the atom in the Schwarzschild–de Sitter, which is observed by the stationary observer at the point where the shift function (velocity) in the Arnowitt–Deser–Misner formalism changes sign. This activation temperature does not depend on the black hole mass and is fully determined by the Hubble parameter, TSdS = $$\sqrt 3 $$H/π. This temperature is twice the Bousso–Hawking temperature TBH, which characterizes the limit of degenerate Lorentzian Schwarzschild–de Sitter universe, when the cosmological and black hole horizons are close to each other, TSdS = 2TBH.The similar doubling of the temperature of Hawking radiation is known in the pure de Sitter spacetime, where the corresponding local temperature describing the ionization of atoms is twice the Gibbons–Hawking temperature, TdS = 2TGH = H/π. We suggest that the activation temperature TdS can be considered as the thermodynamic temperature of the de Sitter state, which determines the local entropy in this state, s = 3H/4G.

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Painlevé–Gullstrand coordinates for Schwarzschild–de Sitter spacetime

Cited by 5 publications

References 52 publications

A trick for calculating surface gravities of Killing horizons

A trick for calculating surface gravities of Killing horizons

Tetrad formalism in the solution of spherically symmetric spacetime in general relativity

On the Global Temperature of the Schwarzschild–de Sitter Spacetime

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