However, these energies could occur in the Early Universe. The Cosmic Timeline Physics gives us a framework within which to describe the events of the Big Bang from the earliest phases to the present. Particle accelerators probe matter at states similar to some of these early phases. Expansion greatly slows down after this brief burst of inflation. Inflation helps to explain why the Universe is so very smooth on large scales.
All forces are now separate.
As the Universe continues to cool, conditions will soon become right for matter to begin to exist in free form, instead of in a soup of matter and photons in equilibrium. Free neutrons are stable at this epoch. Decay into protons, electrons, and neutrinos Left with about 1 neutron for every 7 protons. B We cannot observe this directly, but we can look for the products of these events. Before this, the Universe is opaque.