Abstract
In loop quantum cosmology, a difference equation for the wavefunction describes the evolution of a universe model. This is different from the differential equations that arise in Wheeler–DeWitt quantizations, and some aspects of general properties of solutions can appear differently. Properties of particular interest are boundedness and the presence of small-scale oscillations. Continued fraction techniques are used to show in different matter models the presence of special initial conditions leading to bounded solutions, and an explicit expression for these initial values is derived.
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