Abstract
We clarify a number of issues that arise when extending the analysis of Strong Cosmic Censorship (SCC) to perturbations of highly charged Reissner-Nordstr\"{o}m de Sitter (RNdS) spacetimes. The linear stability of the Cauchy horizon can be determined from the spectral gap of quasinormal modes, thus giving a clear idea of the ranges of parameters that are likely to lead to SCC violations for infinitesimally small perturbations. However, the situation becomes much more subtle once nonlinear backreaction is taken into account. These subtleties have created a considerable amount of confusion in the literature regarding the conclusions one is able to derive about SCC from the available numerical simulations. Here we present new numerical results concerning charged self-gravitating scalar fields in spherical symmetry, correct some previous claims concerning the neutral case, and argue that the existing numerical codes are insufficient to draw conclusions about the potential failure of SCC for near extremal RNdS black hole spacetimes.
Highlights
Strong Cosmic Censorship (SCC) conjectures that Cauchy Horizons (CHs) – the boundaries of the maximal evolution of initial data via the Einstein field equations – are unstable and give rise, upon perturbation, to singular boundaries where the Einstein field equations break down.It is important to clarify how strong these singular boundaries must become in order to correspond to terminal boundaries for the validity of the field equations
The linear stability of the Cauchy horizon can be determined from the spectral gap of quasinormal modes, giving a clear idea of the ranges of parameters that are likely to lead to SCC violations for infinitesimally small perturbations
The numerical results in [5] suggest that this blow up does not occur for highly charged/near extremal Reissner-Nordstrom de Sitter (RNdS) black holes (BHs), i.e. the CHs in these
Summary
Strong Cosmic Censorship (SCC) conjectures that Cauchy Horizons (CHs) – the boundaries of the maximal evolution of initial data via the Einstein field equations – are unstable and give rise, upon perturbation, to singular boundaries where the Einstein field equations break down.It is important to clarify how strong these singular boundaries must become in order to correspond to terminal boundaries for the validity of the field equations. Raimon Luna,1 Miguel Zilhao,2 Vitor Cardoso,2 Joao L.
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