  The dynamics of our universe is characterised by the density parameters for
cosmological constant ($\Omega_V$), nonbaryonic darkmatter($\Omega_{\rm
wimp}$), radiation ($\Omega_R$) and baryons ($\Omega_B$). To these parameters
-- which describe the smooth background universe -- one needs to add at least
another dimensionless number ($\sim 10^{-5}$) characterising the strength of
primordial fluctuations in the gravitational potential, in order to ensure
formation of structures by gravitational instability.
  I discuss several issues related to the description of the universe in terms
of these numbers and argue that we do not yet have a fundamental understanding
of these issues.
