The formation of cosmic structure with modified Newtonian dynamics

I consider the growth of inhomogeneities in a low-density baryonic, vacuum energy-dominated universe in the context of modified Newtonian dynamics (MOND). Such a model cosmology is consistent with the BOOMERanG observations of anisotropies in the CMB (McGaugh 2000). With MOND, the equation for the evolution of spherically symmetric over-densities is non-linear and implies very rapid growth even in a low-density background. Small comoving scales enter the MOND regime earlier than larger scales and therefore evolve to large over-densities sooner. Taking the initial COBE-normalized power spectrum provided by CMBFAST (Seljak & Zeldarriaga 1996), I find that the final power spectrum resembles that of the standard $\Lambda$CDM universe and thus retains the empirical successes of that model