  Quantum cosmology uses a wave function to model the universe, but finding
solutions for this poses a problem as it is difficult to define the boundary
conditions or identify the correct path for a path integral. We begin the
discussion by going over various proposals and look at how bubble universe
nucleation can be used as an analogy for the tunneling wave function. We review
how the Hartle-Hawking wave function and tunneling wave functions are
equivalent. This leads into how the transition between the decelerated and
accelerated expansion is formulated as a bounce in connection space. This is
done in a toy model Universe that contains only radiation and a cosmological
constant $\Lambda$. The wave function is a superposition on an incident wave, a
reflected wave, and an evanescent wave; when it is constructed from wave
packets. Using the toy model, we introduce the new concept of the universe
tunneling to a different classical region during this bounce in connection
space. This concept is explored by deriving the wave function of the evanescent
wave $\psi_{ev}$ in order to calculate $|\psi|^2$ to give an indication of the
probability of the universe tunneling to another classical region.
