CMB anisotropies from stochastic bubble nucleation constrain late-time phase transitions to release less than ~1% of dark energy when β/H⋆≲25, much tighter than Hubble-budget limits.
Field theory models for variable cosmological constant
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abstract
Anthropic solutions to the cosmological constant problem require seemingly unnatural scalar field potentials with a very small slope or domain walls (branes) with a very small coupling to a four-form field. Here we introduce a class of models in which the smallness of the corresponding parameters can be attributed to a spontaneously broken discrete symmetry. We also demonstrate the equivalence of scalar field and four-form models. Finally, we show how our models can be naturally embedded into a left-right extension of the standard model.
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Boiling After the Dust Settles: Constraining First-Order Phase Transitions During Dark Energy Domination
CMB anisotropies from stochastic bubble nucleation constrain late-time phase transitions to release less than ~1% of dark energy when β/H⋆≲25, much tighter than Hubble-budget limits.