Evolving Dark Energy with w =/ -1perHall, Lawrence J.perNomura, YasunoriperOliver, Steven J.orgLawrence Berkeley National Laboratory. Physics Division.Ernest Orlando Lawrence Berkeley National Laboratory, Berkeley, CA (United States)Berkeley, CaliforniaLawrence Berkeley National Laboratory2005-03-31engTheories of evolving quintessence are constructed that generically lead to deviations from the w = -1 prediction of non-evolving dark energy. The small mass scale that governs evolution, m_\phi \approx 10^-33 eV, is radiatively stable, and the"Why Now?'' problem is solved. These results rest crucially on seesaw cosmology: in broad outline, fundamental physics and cosmology can be understood from only two mass scales, the weak scale, v, and the Planck scale, M. Requiring a scale of dark energy \rho_DE^1/4 governed by v^2/M, and a radiatively stable evolution rate m_\phi given by v^4/M^3, leads to a distinctive form for the equation of state w(z) that follows from a cosine quintessence potential. An explicit hidden axion model is constructed. Dark energy resides in the potential of the axion field which is generated by a new QCD-like force that gets strong at the scale \Lambda \approx v^2/M \approx \rho_DE^1/4. The evolution rate is given by a second seesaw that leads to the axion mass, m_\phi \approx \Lambda^2/f, with f \approx M.Radiative Correction, StabilityNumerical CalculationsForecastingPotential, AxionCosmologyQuintessenceDark Energy72Seesaw ModelPhysics Dark EnergySymmetry BreakingAxions