  (Abridged) We present a study of the structure and dynamics of the Corona
Borealis Supercluster (z ~ 0.07) based on the redshifts for 528 galaxies in the
supercluster. The galaxy distribution within Corona Borealis is clumpy and
appears overall to be far from relaxed. A background supercluster at z ~ 0.11
makes a substantial contribution to the projected surface density of galaxies
in the Corona Borealis field. In order to estimate the mass of the
supercluster, we have assumed that the mass of the supercluster is proportional
to v^2r, where v and r are suitable scale velocity and radius, respectively,
and we have used N-body simulations of both critical- and low-density universes
to determine the applicability of standard mass estimators based on this
assumption. Although superclusters are obviously not in equilibrium, our
simulations demonstrate that the virial mass estimator yields mass estimates
with an insignificant bias and a dispersion of only ~25% for objects with
overdensities >~ 5. Non-uniform spatial sampling can, however, cause systematic
underestimates by as much as 30%. All of our simulated superclusters turn out
to be bound, and based on the overdensity of the Corona Borealis supercluster,
we believe it is also very likely to be bound and may well have started to
collapse. The mass of Corona Borealis is at least 3 x 10^16 solar masses, which
yields a B(AB)-band mass-to-light ratio of 564h (M/L)_solar on scales of ~20
h^-1 Mpc. The background supercluster has a mass-to-light ratio of 726h
(M/L)_solar. By comparing the supercluster mass-to-light ratios with the
critical mass-to-light ratio required to close the universe, we determine that
Omega_0 >~ 0.4 on supercluster scales.
