This question is a bit strange, and I tend to agree with Anna that this is related to thermodynamics. The entropy involved here is an entanglement entropy. Suppose you have system A and system B which form an entanglement. The entanglement entropy of system A is $$ S_A~=~-Tr[\rho_A log\rho_A], $$ which equals the entanglement entropy of system B. If the two systems form a pure state then $S_{A+B}~=~0$. The entanglement entropy comes from the fact you have access to only one part of the density matrix $\rho~=~\rho_A\otimes\rho_B$.

This plays a role in cosmology at large. During inflation the vacuum energy density was huge. The cosmological constant $\Lambda~\simeq~(8\pi G/c^4)\rho$, is very large and drives a rapid exponential expansion of space. There is some theoretical controversy here, but while the energy density of the vacuum was very large, the entropy was not that large. The entropy is a measure of the number, N, of degrees of freedom in a system that are coarse grained into a macrostate $S~=~k log(N)$. The other oddball factor is that while the temperature was high, the entropy was low due to the negative heat capacity of event horizons in spacetime. During inflation the event horizon was smaller than a proton, and the entropy is proportional to the area of the horizon $S~=~k A/4L_p^2$.

The bang came about because the exponential expansion rapidly came to a halt, the cosmological constant dropped to a small value (the vacuum energy dropped enormously) and the cosmological horizon adjusted to a very large value. It is now out about $10^{10}$ light years. This means a relatively small number of degrees of freedom enter into complicated entanglements which are not accessible in a local region. The entanglement entropy increases, and these states appear in a highly thermalized form. This is the bang and fire of the big bang. It is a form of latent heat of fusion in a phase transition. The large vacuum energy $\rho~\simeq~10^{100}GeV^4$ crashed into about 10 GeV^4, and the energy gap assumed the form of a thermalized gas of particles.

This was the initial generation of a huge amount of entropy in the early universe. Subsequently entropy is in the form of black holes, radiation and so forth. It is interesting to think we can understand this all from the perspective of quantum mechanics. Into the future the universe will end up as a de Sitter vacuum. In the question:

de Sitter cosmological limit

I indicated how the universe will over a vast period of time will decay from the de Sitter vacuum configuration with a small vacuum energy to a Minkowski spacetime. The horizon will retreat of to “infinity,” which means the entropy becomes infinite. It might be problematic to think of infinite entropy. There might be some sort of cut-off in this process. On the other hand this is just a measure of how the vacuum decays away to zero and there is no energy. The retreat of the cosmological horizon off to infinity is probably a measure of continued quantum entanglement process, which proceeds almost indefnately.

This question is a bit strange, and I tend to agree with Anna that this is related to thermodynamics. The entropy involved here is an entanglement entropy. Suppose you have system A and system B which form an entanglement. The entanglement entropy of system A is $$ S_A~=~-Tr[\rho_A log\rho_A], $$ which equals the entanglement entropy of system B. If the two systems form a pure state then $S_{A+B}~=~0$. The entanglement entropy comes from the fact you have access to only one part of the density matrix $\rho~=~\rho_A\otimes\rho_B$.

This plays a role in cosmology at large. During inflation the vacuum energy density was huge. The cosmological constant $\Lambda~\simeq~(8\pi G/c^4)\rho$, is very large and drives a rapid exponential expansion of space. There is some theoretical controversy here, but while the energy density of the vacuum was very large, the entropy was not that large. The entropy is a measure of the number, N, of degrees of freedom in a system that are coarse grained into a macrostate $S~=~k log(N)$. The other oddball factor is that while the temperature was high, the entropy was low due to the negative heat capacity of event horizons in spacetime. During inflation the event horizon was smaller than a proton, and the entropy is proportional to the area of the horizon $S~=~k A/4L_p^2$.

The bang came about because the exponential expansion rapidly came to a halt, the cosmological constant dropped to a small value (the vacuum energy dropped enormously) and the cosmological horizon adjusted to a very large value. It is now out about $10^{10}$ light years. This means a relatively small number of degrees of freedom enter into complicated entanglements which are not accessible in a local region. The entanglement entropy increases, and these states appear in a highly thermalized form. This is the bang and fire of the big bang. It is a form of latent heat of fusion in a phase transition. The large vacuum energy $\rho~\simeq~10^{100}GeV^4$ crashed into about 10 GeV^4, and the energy gap assumed the form of a thermalized gas of particles.

This was the initial generation of a huge amount of entropy in the early universe. Subsequently entropy is in the form of black holes, radiation and so forth. It is interesting to think we can understand this all from the perspective of quantum mechanics. Into the future the universe will end up as a de Sitter vacuum. In the question:

de Sitter cosmological limit

I indicated how the universe will over a vast period of time will decay from the de Sitter vacuum configuration with a small vacuum energy to a Minkowski spacetime. The horizon will retreat of to “infinity,” which means the entropy becomes infinite. It might be problematic to think of infinite entropy. There might be some sort of cut-off in this process. On the other hand this is just a measure of how the vacuum decays away to zero and there is no energy. The retreat of the cosmological horizon off to infinity is probably a measure of continued quantum entanglement process, which proceeds almost indefnately.