In cosmology, dark energy is a hypothetical form of energy which permeates all of space and has strong negative pressure. According to the theory of relativity, the effect of such a negative pressure is qualitatively similar to a force acting in opposition to gravity at large scales.
Invoking such an effect is currently the most popular method for explaining recent observations that the universe appears
to be expanding at an accelerating rate, as well as accounting for a significant portion of the missing mass in the universe.
Two proposed forms for dark energy are the cosmological constant, a constant energy density filling space homogeneously, and quintessence, a dynamic field whose energy density can vary in time and space. Distinguishing between the alternatives requires high-precision
measurements of the expansion of the universe to understand how the speed of the expansion changes over time. The rate of
expansion is parameterized by the cosmological equation of state. Measuring the equation of state of dark energy is one of the biggest efforts in observational cosmology today.
Adding a cosmological constant to the standard theory of cosmology (i.e. the FLRW metric) has led to a model for cosmology known as the Lambda-CDM model. This model agrees closely with established cosmological observations.
The term dark energy was coined by Michael Turner.
Evidence for dark energy
During the late 1990s, observations of type Ia supernovae suggested that the expansion of the universe is accelerating. These observations have been corroborated by several independent sources. Since then, measurements of the
cosmic microwave background, gravitational lensing, and the large scale structure of the cosmos as well as improved measurements of supernovae have been consistent with the Lambda-CDM model.
The type Ia supernovae provide the most direct evidence for dark energy. Measuring the velocity of receding objects
is accomplished easily by measuring the redshift of the receding object. Finding the distance to an object is a more difficult problem, however. It is necessary to find standard candles: objects for which the absolute magnitude is known, so that it is possible to relate the apparent magnitude to the distance. Without standard candles, it is impossible to measure the redshift-distance relation of Hubble's law. Type Ia supernovae are the best known standard candles for cosmological observation, because they are very bright
and ignite only when the mass of an old white dwarf star reaches the precisely defined Chandrasekhar limit. The distances to the supernovae are plotted against their velocities, and this is used to measure the expansion history
of the universe. These observations indicate that the universe is not decelerating, which would be expected for a matter-dominated
universe, but rather is mysteriously accelerating. These observations are explained by postulating a kind of energy with negative
pressure (see equation of state (cosmology) for a mathematical explanation): dark energy.
The existence of dark energy, in whatever form, also solves the so-called "missing mass" problem. Measurements of the cosmic microwave background (CMB), most recently by the WMAP satellite, indicate that the universe is very close to flat. For the shape of the universe to be flat, the mass/energy density of the Universe must be equal to a certain critical density. The total amount of matter in the Universe (including baryons and dark matter), as measured by the CMB, accounts for only about 30% of the critical density. This implies the existence of an additional
form of energy to account for the remaining 70%.
The theory of large scale structure, which governs the formation of structure in the universe (stars, quasars, galaxies and galaxy clusters), also suggests that the density of matter in the universe is only 30% of the critical density.
The most recent figures from WMAP observations give: 74% dark energy, 22% dark matter, and 4% ordinary matter.
Nature of dark energy
As this NASA chart indicates, 70 percent or more of the universe consists of dark energy, about which we know next to
The exact nature of this dark energy is a matter of speculation. It is known to be very homogeneous, not very dense and presumably does not interact strongly through any of the fundamental forces other than gravity. Since it is not very dense—roughly 10−29 grams per cubic centimeter—it is hard to imagine experiments
to detect it in the laboratory (but see the references for a claimed detection). Dark energy can only have such a profound
impact on the universe, making up 70% of all energy, because it uniformly fills otherwise empty space. The two leading models
are quintessence and the cosmological constant.
The simplest explanation for dark energy is that it is simply the energy of virtual particles mathematically required by uncertainty principle.
This energy is usually labeled as a cosmological constant (termes as Lambda (hence Lambda-CDM model) after the mathematical symbol used to represent it, the Greek letter Λ). Since any energy has mass (energy and mass
are related by E = mc2) this energy (as any other) has a gravitational
Virtual particles energy is sometimes called a vacuum energy or zero-point energy -because it is the energy density of empty vacuum space. Most theories of particle physics mathematically require the existence of vacuum fluctuations that would give the vacuum exactly this sort of energy. The cosmological constant is estimated by cosmologists to be on the
order of 10−29g/cm3, or about 10−120 in reduced Planck units.
Because pressure and energy density are the same quantities, the cosmological constant of expanding space must have negative
pressure equal to its energy density and so causes the expansion of the universe to accelerate (see equation of state (cosmology)). The reason why a cosmological constant has negative pressure can be seen from classical thermodynamics. The work done by
a change in volume dV is equal to −p dV, where p is the pressure. But the amount of energy
in a box of vacuum energy actually increases when the volume increases (dV is positive), because the energy is equal
to ρV, where ρ is the energy density of the cosmological constant. Therefore, p is negative
and, in fact, p = −ρ.
A major problem is that some quantum field theories predict large cosmological constant. Some supersymmetric theories which do not account for virtual particles require a cosmological constant that is exactly zero.
In spite of its problems, the zero point energy of virtual particles explains the acceleration of space best - just one
number successfully explains a multitude of observations. Thus, the current standard model of cosmology, the Lambda-CDM model,
includes the cosmological constant as an essential feature.
Alternatively, dark energy might arise from the particle-like excitations in some type of dynamical field, referred to as quintessence. Quintessence differs from the cosmological constant in that it can vary in space and time. In order for it not to clump
and form structure like matter, it must be very light so that it has a large Compton wavelength.
No evidence of quintessence is yet available, but it cannot be ruled out either. It generally predicts a slightly slower
acceleration of the expansion of the universe than the cosmological constant. Some workers think that the best evidence for
quintessence would come from violations of Einstein's equivalence principle and variation of the fundamental constants in space or time. Scalar fields are predicted by the standard model and string theory, but an analogous problem to the cosmological constant problem (or the problem of constructing models of cosmic inflation) occurs: renormalization theory predicts that scalar fields should acquire large masses.
The cosmic coincidence problem asks why the cosmic acceleration began when it did. If cosmic acceleration began earlier in the universe, structures
such as galaxies would never have had time to form and life, at least as we know it, would never have had a chance to exist. Proponents of
the anthropic principle view this as support for their arguments. However, many models of quintessence have a so-called tracker behavior,
which solves this problem. In these models, the quintessence field has a density which closely tracks (but is less than) the
radiation density until matter-radiation equality, which triggers quintessence to start behaving as dark energy, eventually dominating the universe. This naturally sets the
low energy scale of the dark energy.
Some special cases of quintessence are phantom energy, in which the energy density of quintessence actually increases with time, and k-essence (short for kinetic quintessence)
which has a non-standard form of kinetic energy. They can have unusual properties: phantom energy, for example, can cause a Big Rip.
Some theorists think that dark energy and cosmic acceleration are a failure of general relativity on very large scales, larger than superclusters. It is a tremendous extrapolation to think that our law of gravity, which works so well in the solar system, should work without correction on the scale of the universe. However, most attempts at modifying general relativity have turned out either to be equivalent to theories of quintessence, or are inconsistent with observations.
Other ideas for dark energy have come from string theory, brane cosmology and the holographic principle, but have not yet proved as compelling as quintessence and the cosmological constant.
Implications for the fate of the universe
Cosmologists estimate that the acceleration began to outperform gravity on cosmological scale roughly 5 billion years ago. Before that, it is thought that the expansion was decelerating, due to the attractive influence
of dark matter and baryons. The density of dark matter in an expanding universe disappears more quickly than dark energy, and eventually the dark energy
dominates. Specifically, when the volume of the universe doubles, the density of dark matter is halved but the density of dark energy is nearly unchanged (it is exactly constant in the case of a cosmological constant).
If the acceleration continues indefinitely, the ultimate result will be that galaxies outside the local supercluster will move beyond the cosmic horizon: they will no longer be visible, because their relative speed becomes greater than the speed of light. This is not a violation
of special relativity, and the effect cannot be used to send a signal between them. (Actually there is no way to even define "relative speed" in
a curved spacetime. Relative speed and velocity can only be meaningfully defined in flat spacetime or in sufficiently small
(infinitesimal) regions of curved spacetime). Rather, it prevents any communication between them and the objects pass out
of contact. The Earth, the Milky Way and the Virgo supercluster, however, would remain virtually undisturbed while the rest of the universe recedes. In this scenario, the local supercluster
would ultimately suffer heat death, just as was thought for the flat, matter-dominated universe, before measurements of cosmic acceleration.
There are some very speculative ideas about the future of the universe. One suggests that phantom energy causes divergent
expansion, which would imply that the effective force of dark energy continues growing until it dominates all other forces
in the universe. Under this scenario, dark energy would ultimately tear apart all gravitationally bound structures, including
galaxies and solar systems, and eventually overcome the electrical and nuclear forces to tear apart atoms themselves, ending the universe in a Big Rip. On the other hand, dark energy might dissipate with time, or even become attractive. Such uncertainties leave open the possibility
that gravity might yet rule the day and lead to a universe that contracts in on itself in a "Big Crunch". Some scenarios, such as the cyclic model suggest this could be the case. While these ideas are not supported by observations, they are not ruled out. Measurements
of acceleration are crucial to determining the ultimate fate of the universe in big bang theory.
The cosmological constant was first proposed by Einstein as a mechanism to obtain a stable solution of the gravitational field equation that would lead to a static universe, effectively using dark energy to balance gravity. Not only was the mechanism an inelegant
example of fine-tuning, it was soon realized that Einstein's static universe would actually be unstable because local inhomogeneities would ultimately
lead to either the runaway expansion or contraction of the universe. The equilibrium is unstable: if the universe expands slightly, then the expansion releases vacuum energy, which causes yet more expansion.
Likewise, a universe which contracts slightly will continue contracting. These sorts of disturbances are inevitable, due to
the uneven distribution of matter throughout the universe. More importantly, observations made by Edwin Hubble showed that the universe appears to be expanding and not static at all. Einstein famously referred to his failure to predict
the idea of a dynamic universe, in contrast to a static universe, as his greatest blunder. Following this realization, the
cosmological constant was largely ignored as a historical curiosity.
Alan Guth proposed in the 1970s that a negative pressure field, similar in concept to dark energy, could drive cosmic inflation in the very early universe. Inflation postulates that some repulsive force, qualitatively similar to dark energy, resulted
in an enormous and exponential expansion of the universe slightly after the Big Bang. Such expansion is an essential feature of most current models of the Big Bang. However, inflation must have occurred at
a much higher energy density than the dark energy we observe today and is believed to have completely ended when the universe
was just a fraction of a second old. It is unclear what relation, if any, exists between dark energy and inflation. Even after
inflationary models became accepted, the cosmological constant was believed to be irrelevant to the current universe.
By 1998, the missing mass problem of big bang nucleosynthesis and large scale structure was established, and some cosmologists had started to theorize that there was an additional component to our universe, with
properties very similar to dark energy. This suspicion was reinforced by supernova observations of accelerated expansion,
simultaneously released by the teams of Riess et al and Perlmutter et al. This resulted in the Lambda-CDM model, which as of 2005 has remained consistent with a series of increasingly rigorous cosmological observations, the latest being the 2005 Supernova
Legacy Survey.  First results from the SNLS reveal that dark energy behaves like Einstein's cosmological constant to a precision of 10 per