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Observations of clusters gives a total matter density $\Omega_{\mathrm{M}} \simeq 0.3$. At the same time observation of the microwave background indicates a flat Universe $\Omega_0=1$. There must, therefore, be another source of mass energy that does not cluster to make up the difference, the dark energy $\Omega_{\mathrm{d}}$ (now) $\simeq 0.7$. This mass density cannot have been dominant in the past otherwise it would have prevented the formation of structure, so it must grow with time relative to the matter density. Use local energy conservation and the equation of state $P=w \rho c^2$ to show that, at time $t$, $$ \rho_{\mathrm{d}} R^{3(\beta+1)}=\text { constant, } $$ where $\beta=P /\left(\rho c^2\right)$. By considering the ratio $\Omega_{\mathrm{d}} / \Omega_{\mathrm{m}}$ deduce that the pressure of the dark energy must be negative. (This makes the vacuum energy or quintessence a candidate for the dark energy.)

   Observations of clusters gives a total matter density $\Omega_{\mathrm{M}} \simeq 0.3$. At the same time observation of the microwave background indicates a flat Universe $\Omega_0=1$. There must, therefore, be another source of mass energy that does not cluster to make up the difference, the dark energy $\Omega_{\mathrm{d}}$ (now) $\simeq 0.7$. This mass density cannot have been dominant in the past otherwise it would have prevented the formation of structure, so it must grow with time relative to the matter density. Use local energy conservation and the equation of state $P=w \rho c^2$ to show that, at time $t$,
$$
\rho_{\mathrm{d}} R^{3(\beta+1)}=\text { constant, }
$$
where $\beta=P /\left(\rho c^2\right)$. By considering the ratio $\Omega_{\mathrm{d}} / \Omega_{\mathrm{m}}$ deduce that the pressure of the dark energy must be negative. (This makes the vacuum energy or quintessence a candidate for the dark energy.)

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An introduction to the science of cosmology
An introduction to the science of cosmology
Derek Raine, E.G.… 2nd Edition
Chapter 9, Problem 6 ↓

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The conservation of energy-momentum tensor gives us the continuity equation: \[ \frac{d}{dt}(\rho R^3) + P \frac{d}{dt}(R^3) = 0, \] where \(\rho\) is the energy density, \(R\) is the scale factor, and \(P\) is the pressure.  Show more…

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Observations of clusters gives a total matter density $\Omega_{\mathrm{M}} \simeq 0.3$. At the same time observation of the microwave background indicates a flat Universe $\Omega_0=1$. There must, therefore, be another source of mass energy that does not cluster to make up the difference, the dark energy $\Omega_{\mathrm{d}}$ (now) $\simeq 0.7$. This mass density cannot have been dominant in the past otherwise it would have prevented the formation of structure, so it must grow with time relative to the matter density. Use local energy conservation and the equation of state $P=w \rho c^2$ to show that, at time $t$, $$ \rho_{\mathrm{d}} R^{3(\beta+1)}=\text { constant, } $$ where $\beta=P /\left(\rho c^2\right)$. By considering the ratio $\Omega_{\mathrm{d}} / \Omega_{\mathrm{m}}$ deduce that the pressure of the dark energy must be negative. (This makes the vacuum energy or quintessence a candidate for the dark energy.)
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Key Concepts

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Dark Energy
Dark energy is a form of energy that appears to fill the universe and does not cluster like ordinary matter. Crucially, it is characterized by a negative pressure, which contributes to the accelerated expansion of the universe. While its exact nature is still under investigation, its presence is inferred from discrepancies between the observed matter density and the critical density required for a flat universe.
Equation of State
The equation of state in cosmology is a relationship that connects the pressure (P) of a cosmic fluid with its energy density (?) through a parameter (w), expressed as P = w ? c². This relationship determines how the energy density evolves as the universe expands and plays a critical role in distinguishing between different components, such as matter (typically w = 0) and dark energy (w < 0).
Local Energy Conservation
Local energy conservation in an expanding universe is encapsulated by the continuity equation, which governs the evolution of the energy density as the universe expands. When combined with the equation of state, it shows that for any component, the product ? R^(3(?+1)) remains constant (with ? = w). This relationship indicates how the energy density dilutes with the scale factor (R), thereby allowing us to track the relative contribution of different cosmic components over time.
Scale Factor
The scale factor, often denoted by R, is a measure of the size of the universe at a given time relative to a chosen reference time. It is an essential concept in cosmology because it quantifies the expansion of space. The evolution of various energy densities (for matter, radiation, or dark energy) is directly related to changes in the scale factor, as described by the relation derived from local energy conservation.
Negative Pressure
Negative pressure is an unusual property that is essential for explaining the behavior of dark energy. Unlike normal matter, which typically exerts positive pressure, a negative pressure results in a repulsive gravitational effect. This negative pressure is crucial for driving the accelerated expansion of the universe, supporting the notion that the dark energy component must have such a characteristic to reconcile observations of cosmic structure with a flat universe.

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