 A second type of scenario according to which future developments in physics may eliminate at least some fine-tuning for life would be a dynamical account of the generation of life-friendly conditions, in analogy to the Darwinian “dynamical” evolutionary account of biological fine-tuning for survival and reproduction. Inflationary cosmology (Guth 1981, 2000) is a paradigm candidate example of such an account in that it dynamically explains why the total cosmic energy density \(\Omega\) in the early universe is extremely close to the so-called critical value \(\Omega_c\) (see  Section 1.1)—or,  equivalently, why the overall spatial curvature of the universe is close to zero. According to inflationary cosmology, the very early universe undergoes a period of exponential or near-exponential expansion (“inflation”) which effectively flattens out space and results in near-zero post-inflation curvature, leading to a total energy density \(\Omega\) extremely close to the critical density \(\Omega_c\). Further claimed achievements of inflationary cosmology include its ability to account for the observed near-perfect isotropy of the universe and the absence of magnetic monopoles. The strongest empirical support for inflationary cosmology, however, is now widely believed to come from of its apparently correct predictions of the shape of the cosmic microwave background fluctuations (PLANCK collaboration 2014).