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Nonradial stability of topological stars
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Topological stars are regular, horizonless solitons arising from dimensional compactification of Einstein-Maxwell theory in five dimensions, which could describe qualitative properties of microstate geometries for astrophysical black holes. They also provide a compelling realization of ultracompact objects arising from a well-defined theory and display all the phenomenological features typically associated with black hole mimickers, including a (stable) photon sphere, long-lived quasinormal modes, and echoes in the ringdown. By completing a thorough linear stability analysis, we provide strong numerical evidence that these solutions are stable against nonradial perturbations with zero Kaluza-Klein momentum.
Forward citations
Cited by 2 Pith papers
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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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