When the universe expands, it is important to understand that how its energy content evolves depends on the form of energy involved. If all that energy is locked up in the form of mass energy, then the density of that matter will decrease proportionally to the relative increase of any arbitrary volume of the universe (i.e. if expansion doubles the size of things, all volumes will be multiplied by 8, and correspondingly all densities will be divided by 8). In other words, if $a$ is the scale factor of the universe, and $\rho_m$ its matter density, we have :
$$
\rho_m \propto a^{-3}
$$
Hence, the total amount of mass energy (which is $\rho_m \times a^3$) is conserved. What happens if the energy content of the universe is dominated by radiation ? In that situation, on top of the decrease in density, radiation is also redshifted proportionally to the scale factor. Hence, if $\rho_R$ is the radiation energy density, we have :
$$
\rho_R \propto a^{-4}
$$
Here, the total energy ($\rho_R \times a^3$) is not conserved, which, remember, is not a problem in General Relativity. The period your textbook is referring to is likely the radiation era (roughly the first $50,000$ years of the universe's history). Indeed, during this time, the universe cooled in a way that decreased the total energy of the universe. It didn't go anywhere, it is indeed "lost" in a sense.
Conversely, we can have a situation where energy is gained. This is the case for any dark energy model, but let's keep it simple and consider the case of a cosmological constant $\Lambda$. This corresponds to a constant energy density. That is to say $\rho_\Lambda$ is independent of $a$. The total energy will then be $\rho_\Lambda \times a^3$, and will therefore increase with expansion.
Here I loosely used the word "total" given that it doesn't mean much in an infinite universe. A more rigorous expression for "total" would be any arbitrarily chosen sphere in comoving coordinates, so long as its radius is above the inhomogeneity scale.
The expansion of the Universe is driven by the dominant forms of energy and matter density. This is essentially an expression of a famous statement by John Wheeler (from memory, apologies if I get the exact wording wrong): "Spacetime tells matter how to move, matter tells spacetime how to curve". In this case, the matter is telling the Universe how to expand. Mathematically, Einstein's equations describing gravity, when restricted to homogeneous and isotropic Universes (relevant for cosmology), reduce to the Friedmann equations which relate the expansion rate to the matter content.
There are lots of different kinds of energy density, but for cosmology there (to zeroth order) three that really matter:
- When the Universe is dominated by non-relativistic matter (atoms and molecules but also dark matter), the size of the Universe grows with time as approximately $\sim t^{2/3}$.
- When the Universe is dominated by relativistic matter (such as photons or a very hot gas of particles moving relativistically), the Universe grows as $\sim t^{1/2}$.
- When the Universe is dominated by an approximately constant energy density (more on this in a minute), the Universe grows exponentially as $\sim e^{Ht}$, where $H$ is the expansion rate.
Note that ordinary matter (relativistic and non-relativistic) do not have a constant energy density. As the Universe expands, the energy density (energy per unit volume) goes down, because there are the same number of particles but a larger volume. (Well, it can be that the number of particles changes, but at the level of this discussion that's a detail that is not so important, the key thing is that the energy per unit volume decreases for ordinary matter).
So something weird is needed in order to provide constant energy density as the Universe expands. Physically we can imagine that there is a certain amount of energy associated with every volume of space -- then as space expands, in a sense creating more space, there is also more energy associated with that space. This is essentially the cosmological constant. Another possibility is that there is a dynamical field (a "scalar field") which permeates space, and an associated potential energy that is approximately the same anywhere.
With all that background, the current generally accepted model of cosmology is that:
- The energy density is initially dominated in some scalar field, whose large potential energy permeates space and causes exponential expansion.
- The scalar field rolls down its potential, and eventually rolls to an area of its potential where its potential energy is very small. During this process, the scalar field transfers its energy to ordinary matter and radiation fields.
- The Universe enters a phase where it is dominated by relativistic, hot matter.
- Eventually the Universe cools to a point where the matter that dominates the energy budget is non-relativistic, so the growth rate changes.
- As the Universe cools even further, and its energy density lowers, eventually the energy density of the Universe becomes dominated by a small constant value that was likely present all along, but (up until recently) was only a negligible contribution to the overall budget. This last component is what was discovered in the late 90s as the accelerated expansion of the Universe.
While this is sort of a standard picture, not all points are on equally solid footing. The first two bullet points are not universally accepted. The first bullet point is called "inflation", and (if true) explains why the Universe we see is spatially flat, and why we observe the CMB to be at the same temperature, even though the different patches that make up the CMB were not in causal contact with each other before the Big Bang in models without inflation. The inflationary period also explains the origin of the spectrum of the CMB. The second bullet point is a mysterious process that is thought to involve some combination of the decay of scalar particles into other matter ("reheating") or some dynamical process where the scalar field coherently pumps energy into other fields ("preheating").
Points 3-5, however, are on quite solid observational footing. We have observations throughout the Universe's history that probe the Universe during these different eras. While we do not fully understand what is driving the Universe today, a perfectly satisfactory model that explains all the observations is that there is a very small constant energy density that has always been pervading the Universe throughout its entire history, but we are only seeing it now because we had to wait until the Universe became dilute enough to see its effects.
Best Answer
Here is the scenario from wikipedia
Note that before 10^-35 seconds the inflation is the steady one from the original Big Bang.
the rapid inflation results in the increase of kinetic energy as the inflaton field settled to its lower energy level
So it is the time necessary for the inflaton field to fall from the higher to the lower energy level.
The model continues here
So it is the gravitational attraction that takes over once the inflaton field is at its lowest energy state.A lot of kinetic energy ended up as potential gravitational balancing the expansion
and is currently doing so.
As I understand it the subject is still under research, theoretically and experimentally