The discussion explores why solar systems and galaxies appear to rotate on a two-dimensional plane, emphasizing that while orbits are not perfectly planar, they are largely influenced by the initial conditions of their formation from a rotating nebula. The gravitational interactions within a collapsing gas cloud lead to a disc-like structure, as parts of the cloud that interact less tend to remain in a stable orbit. The conversation also touches on the differences between structures like globular clusters and elliptical galaxies, which do not exhibit the same planar characteristics due to their slower rotation and different formation processes. Additionally, the role of angular momentum and energy loss during the collapse of these structures is highlighted, explaining the transition from a spherical to a disc shape. Overall, the discussion underscores the significance of rotational dynamics in shaping the architecture of celestial systems.