Abstract
In the Swampland philosophy of constraining EFTs from black hole mechanics we study charged black hole evaporation in de Sitter space. We establish how the black hole mass and charge change over time due to both Hawking radiation and Schwinger pair production as a function of the masses and charges of the elementary particles in the theory. We find a lower bound on the mass of charged particles by demanding that large charged black holes evaporate back to empty de Sitter space, in accordance with the thermal picture of the de Sitter static patch. This bound is satisfied by the charged spectrum of the Standard Model. We discuss phenomenological implications for the cosmological hierarchy problem and inflation. Enforcing the thermal picture also leads to a heuristic remnant argument for the Weak Gravity Conjecture in de Sitter space, where the usual kinematic arguments do not work. We also comment on a possible relation between WGC and universal bounds on equilibration times. All in all, charged black holes in de Sitter should make haste to evaporate, but they should not rush it.2
Highlights
The ample evidence for some Swampland constraints in string theory gives us confidence they are probably correct, but it is important that at least in some cases we seem to have identified a physical principle underlying the conjecture
The formalism developed in these previous sections provides a means to understand how black holes evaporate in de Sitter space
In flat space and AdS, the Weak Gravity Conjecture is intimately related to Cosmic Censorship and the stability of extremal black holes
Summary
We consider a (3 + 1)-dimensional Einstein-Maxwell-de Sitter system, with action (in − + ++ signature) This theory admits charged black hole solutions, the RN-dS metric, The black hole and the cosmological horizons will have different temperatures, and so they won’t be in thermal equilibrium. The lower branch of the curve in figure 1 is the charged Nariai branch, and it contains subextremal charged black holes with the same area as the cosmological horizon. We will be especially interested in this branch and discuss it in greater detail below These two branches meet at a point, dubbed the “ultracold” black hole [103] since semiclassically it describes an equilibrium configuration at vanishingly small temperature. Stuff closer to the black hole than the geodesic observer will eventually fall in, while stuff further out will keep on receding from the observer towards the cosmological horizon
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