Gravitational vacuum condensate stars

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Abstract
A new final state of gravitational collapse is proposed. By extending the concept of Bose–Einstein condensation to gravitational systems, a cold, dark, compact object with an interior de Sitter condensate p v = -ρ v and an exterior Schwarzschild geometry of arbitrary total mass M is constructed. These regions are separated by a shell with a small but finite proper thickness ℓ of fluid with equation of state p = +ρ , replacing both the Schwarzschild and de Sitter classical horizons. The new solution has no singularities, no event horizons, and a global time. Its entropy is maximized under small fluctuations and is given by the standard hydrodynamic entropy of the thin shell, which is of the order k B ℓ Mc / , instead of the Bekenstein–Hawking entropy formula, S BH = 4 π k B GM 2 / c . Hence, unlike black holes, the new solution is thermodynamically stable and has no information paradox.