Black holes in an expanding universe and supersymmetry

Abstract

This paper analyzes the supersymmetric solutions to five and six-dimensional minimal (un)gauged supergravities for which the bilinear Killing vector constructed from the Killing spinor is null. We focus on the spacetimes which admit an additional SO(1, 1) boost symmetry. Upon the toroidal dimensional reduction along the Killing vector corresponding to the boost, we show that the solution in the ungauged case describes a charged, nonextremal black hole in a Friedmann-Lemaître-Robertson-Walker (FLRW) universe with an expansion driven by a massless scalar field. For the gauged case, the solution corresponds to a charged, nonextremal black hole embedded conformally into a Kantowski-Sachs universe. It turns out that these dimensional reductions break supersymmetry since the bilinear Killing vector and the Killing vector corresponding to the boost fail to commute. This represents a new mechanism of supersymmetry breaking that has not been considered in the literature before.PACS numbers:

Static spacetimes haunted by a phantom scalar field III: asymptotically (A)dS solutions

“…This solution does not admit additional Killing vectors even in the case with a single point source, so that it is genuinely dynamical. Similar dynamical solutions in FLRW universe can be found e.g., in [75][76][77][78][79][80], which describes respectively a single equilibrium black hole in expanding universe. However, the present solution differs from these solutions in that the current metric (A.6) fails to admit any "near-horizon limit," leading to the singular spacetime.…”

“…Since there appear no scalar/p.p curvature singularities in the entire parameter region, the solution indeed describes a wormhole in AdS. The throat exists at (79).…”

Evolving black holes in inflation

“…Such situations are highly interactive involving classical accretion, the expansion of the universe, as well as classical and quantum mechanical radiation exchange. Known analytic solutions include the stationary Kerr-Reissner-Nordstrom de Sitter metric [7], the cosmological McVittie black hole spacetime [8], which has an unphysical pressure field except when it reduces to Schwarzschild-de Sitter [9], and cases of multi, maximally charged, black holes [10][11][12][13] that exploit fake supersymmetries [14,15]. A range of approximations and numerical analyses have been used to study accretion and estimate the growth of black holes in these interactive systems, including .…”

Black hole and cosmological particle production in Schwarzschild de Sitter

“…and (29) for the limiting behaviors of K. The complex phase factor in σ results from the analytic continuation in ω to obtain β b ωω that leads to the decaying exponential in |β b ωω | 2 .…”

“…Features of black hole thermodynamics in deSitter, including approaches to temperature, entropy, and conserved charges, are studied in [14][15][16][17][18][19][20][21][22][23][24][25][26][27][28]. Features of black hole thermodynamics in an expanding universe are contained in [29][30][31]. In addition to the classical gravitational perturbations described by the first laws ( 6) and (7), there are quantum fluctuations in the matter fields, even if the classical values are zero.…”