General Relativity

Wald, Robert M.

doi:10.7208/chicago/9780226870373.001.0001

Cited by 7,937 publications

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“…In classical General Relativity it is commonly accepted that the final state of complete gravitational collapse is a singular state called a 'black hole' [41,66,102]. This object is characterized by a central space-time singularity at r = 0 surrounded by an event horizon, a null hypersurface located at the Schwarzschild radius r S = 2M which separates points connected to infinity by a timelike curve from those that are not.…”

Section: List Ofmentioning

confidence: 99%

“…It is well known that this interior solution shows a divergence in pressure when the radius of the star contracts to R = (9/4)M , known as the Schwarzschild-Buchdahl bound [13,92]. The existence of this limit in addition to the homogeneous mass approximation, considered 'unrealistic', have been assumed to be sufficient reasons to exclude the Schwarzschild star from further investigation [102]. This complete disregard of the interior solution has left the interesting region R s < R < (9/8)R s unexplored.…”

Section: List Ofmentioning

confidence: 99%

“…For cold matter at low densities (low compared to nuclear densities which are of the order of 10 14 g/cm 3 ), the pressure will be provided by quantum mechanical effects (exclusion principle). In the non-relativistic case, the pressure is estimated to be [102] …”

Section: Gravitational Collapsementioning

confidence: 99%

“…A statement which is usually ignored in the literature [14,90,95,102] and only remarked in [52] is that this equivalence between gravitational fields and non-inertial frames is not complete. The difference settles on the behavior at infinity of these fields.…”

Section: Introductionmentioning

confidence: 99%

“…In other words, the equations of physics must be written covariantly in tensorial form. Therefore, the only spacetime quantities that must appear in the laws of physics are the metric g µν and quantities derivable from it [102]. Additionally, we require that in the Lorentz spacetime η µν (flat space) the equations must reduce to their corresponding forms in special relativity.…”

Section: Introductionmentioning

confidence: 99%

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Slowly rotating supercompact Schwarzschild stars

Posada¹

2017

Monthly Notices of the Royal Astronomical Society

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AcknowledgmentsI am grateful to the universe, for its harmony. The project is the study of integral and surface properties of slowly rotating homogeneous masses in the gravastar limit R → R s , where R s is the Schwarzschild radius. For this purpose we followed the perturbative method proposed by Hartle in 1967. In this model, the relativistic equations of structure for a slowly rotating star were derived at second order in the angular velocity Ω. An interesting, and educational, application of this model was investigated by Chandrasekhar and Miller. I am indebted to the Department of Physics andIn their approach, they solved numerically the structure equations of a homogeneous star (constant energy density) up to the Buchdahl bound (9/8)R s . Based on this work, our objective was to investigate the interesting region below the Buchdahl bound R s < R < (9/8)R s , which has not been studied previously in the literature.Our results were astonishing. We found that the surface properties and quadrupole mass moment approach the values corresponding to those of the Kerr metric when expanded at second order in angular momentum. This remarkable result provides a long sought solution to the problem of the source of rotation in the Kerr spacetime.iv

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Section: List Ofmentioning

confidence: 99%

Section: List Ofmentioning

confidence: 99%

Section: Gravitational Collapsementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Slowly rotating supercompact Schwarzschild stars

Posada¹

2017

Monthly Notices of the Royal Astronomical Society

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Hawking radiation from dilaton gravity in 1 + 1 dimensions: a pedagogical review

Kummer¹,

Vassilevich²

1999

Ann. Phys.

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Hawking radiation in d 4 is regarded as a well understood quantum theoretical feature of Black Holes or of other geometric backgrounds with an event horizon. On the other hand, the dilaton theory, emerging after spherical reduction, and generalized dilaton theories only during the last years became the subject of numerous studies which unveiled a surprisingly difficult situation. Recently we have found some solution to the problem of Hawking flux in spherically reduced gravity which has the merit of using a minimal input. It leads to exact cancellation of negative contributions to this radiative flux, encountered in other approaches at infinity, so that our result asymptotically coincides with the one of minimally coupled scalars. The use of an integrated action is avoided Ð although we have been able to present also that quantity in a closed expression. This short review also summarizes and critically discusses recent activities in this field, including the problem of``conformal framesº for the background and questions which seem to be open in our own approach as well as in others.

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Deviations from the Area Law for Supersymmetric Black Holes

2000

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We review modifications of the Bekenstein-Hawking area law for black hole entropy in the presence of higher-derivative interactions. In four-dimensional N = 2 compactifications of string theory or M-theory these modifications are crucial for finding agreement between the macroscopic entropy obtained from supergravity and the microscopic entropy obtained by counting states in string or M-theory. Our discussion is based on the effective Wilsonian action, which in the context of N = 2 supersymmetric theories is defined in terms of holomorphic quantities. At the end we briefly indicate how to incorporate non-holomorphic corrections.

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General Relativity

Cited by 7,937 publications

References 0 publications

Slowly rotating supercompact Schwarzschild stars

Slowly rotating supercompact Schwarzschild stars

Hawking radiation from dilaton gravity in 1 + 1 dimensions: a pedagogical review

Deviations from the Area Law for Supersymmetric Black Holes

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