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Topological Stars and Black Holes
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We study smooth bubble spacetimes in five-dimensional Einstein-Maxwell theory that resemble four-dimensional magnetic black holes upon Kaluza-Klein reduction. We denote them as Topological Stars since they have topological cycles supported by magnetic flux. They can be macroscopically large compared to the size of the Kaluza-Klein circle and could describe qualitative properties of microstate geometries for astrophysical black holes. We also describe five-dimensional black strings without curvature singularity, the interior caps as a two-dimensional Milne space with a bubble.
Forward citations
Cited by 4 Pith papers
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Superradiant amplification by rotating viscous compact objects
Using causal BDNK hydrodynamics, the authors derive coupled gravitational-wave and viscous-mode equations for slowly rotating stars and find superradiant amplification at low frequencies.
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The radial action for massive particles in spherically symmetric geometries: Exact resummation at any PM order
The massive-particle radial action and scattering angle in Schwarzschild, Schwarzschild-Tangherlini and D3-brane geometries are resummed in hypergeometric/Fox-Wright form, and the massive scalar quantum a-cycle is ide...
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Topological Stars and scalar wave equation: Exact resummation of the renormalized angular momentum in the eikonal limit
For Topological Stars, the eikonal-limit renormalized angular momentum is expressed as hypergeometric functions tied to the null geodesic radial action, generalizing the Schwarzschild resummation.
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Scattering angle in a Topological Star spacetime: a self-force approach
An analytic, large-angular-momentum scattering angle for unbound geodesics and scalar self-force in Topological Star spacetime, with an unresolved regulator in the conservative self-force piece.
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