From Wikipedia, the free encyclopedia
In
physical cosmology and
astronomy,
dark energy is an unknown form of
energy which is hypothesized to permeate all of space, tending to
accelerate the
expansion of the universe.
[1] Dark energy is the most accepted hypothesis to explain the observations since the 1990s indicating that the universe is
expanding at an
accelerating rate. According to the
Planck mission team, and based on the
standard model of cosmology, on a
mass–energy equivalence basis, the
observable universe contains 26.8%
dark matter, 68.3% dark energy (for a total of 95.1%) and 4.9%
ordinary matter.
[2][3][4][5] Again on a mass–energy equivalence basis, the density of dark energy (6.91 × 10
−27 kg/m
3)
is very low, much less than the density of ordinary matter or dark
matter within galaxies. However, it comes to dominate the mass–energy of
the universe because it is uniform across space.
[6][7]
Two proposed forms for dark energy are the
cosmological constant, a
constant energy density filling space homogeneously,
[8] and
scalar fields such as
quintessence or
moduli,
dynamic
quantities whose energy density can vary in time and space.
Contributions from scalar fields that are constant in space are usually
also included in the cosmological constant. The cosmological constant
can be formulated to be equivalent to
vacuum energy.
Scalar fields that do change in space can be difficult to distinguish
from a cosmological constant because the change may be extremely slow.
High-precision measurements of the
expansion of the universe are required to understand how the expansion rate changes over time and space. In
general relativity, the evolution of the expansion rate is parameterized by the cosmological
equation of state
(the relationship between temperature, pressure, and combined matter,
energy, and vacuum energy density for any region of space). Measuring
the equation of state for dark energy is one of the biggest efforts in
observational cosmology today.
Adding the cosmological constant to cosmology's standard
FLRW metric leads to the
Lambda-CDM model, which has been referred to as the "
standard model of cosmology"
because of its precise agreement with observations. Dark energy has
been used as a crucial ingredient in a recent attempt to formulate a
cyclic model for the universe.
[9]
Nature of dark energy
Many things about the nature of dark energy remain matters of
speculation. The evidence for dark energy is indirect but comes from
three independent sources:
- Distance measurements and their relation to redshift, which suggest the universe has expanded more in the last half of its life.[10]
- The theoretical need for a type of additional energy that is not matter or dark matter to form the observationally flat universe (absence of any detectable global curvature).
- It can be inferred from measures of large scale wave-patterns of mass density in the universe.
Dark energy is thought to be very
homogeneous, not very
dense and is not known to interact through any of the
fundamental forces other than
gravity. Since it is quite rarefied—roughly 10
−30 g/cm
3—it
is unlikely to be detectable in laboratory experiments. Dark energy can
have such a profound effect on the universe, making up 68% of universal
density, only because it uniformly fills otherwise empty space. The two
leading models are a
cosmological constant and
quintessence. Both models include the common characteristic that dark energy must have negative pressure.
Effect of dark energy: a small constant negative pressure of vacuum
Diagram representing the accelerated expansion of the universe due to dark energy.
Independently of its actual nature, dark energy would need to have a
strong negative pressure (acting repulsively) in order to explain the
observed
acceleration of the
expansion of the universe.
According to general relativity, the pressure within a substance
contributes to its gravitational attraction for other things just as its
mass density does. This happens because the physical quantity that
causes matter to generate gravitational effects is the
stress–energy tensor, which contains both the energy (or matter) density of a substance and its pressure and viscosity. In the
Friedmann–Lemaître–Robertson–Walker metric,
it can be shown that a strong constant negative pressure in all the
universe causes an acceleration in universe expansion if the universe is
already expanding, or a deceleration in universe contraction if the
universe is already contracting. This accelerating expansion effect is
sometimes labeled "gravitational repulsion", which is a colorful but
possibly confusing expression. In fact a negative pressure does not
influence the gravitational interaction between masses—which remains
attractive—but rather alters the overall evolution of the universe at
the cosmological scale, typically resulting in the accelerating
expansion of the universe despite the attraction among the masses
present in the universe. The acceleration is simply a function of dark
energy density. Dark energy is persistent: its density remains constant
(experimentally, within a factor of 1:10), i.e. it does not get diluted
when space expands.
Evidence of existence
Supernovae
A Type Ia supernova (bright spot on the bottom-left) near a galaxy
In 1998, published observations of
Type Ia supernovae ("one-A") by the
High-Z Supernova Search Team[11] followed in 1999 by the
Supernova Cosmology Project[12] suggested that the expansion of the universe is
accelerating.
[13] The 2011
Nobel Prize in Physics was awarded to
Saul Perlmutter,
Brian P. Schmidt and
Adam G. Riess for their leadership in the discovery.
[14][15]
Since then, these observations have been corroborated by several independent sources. 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.
[16]
Some people argue that the only indication for the existence of dark
energy is observations of distance measurements and associated
redshifts. Cosmic microwave background anisotropies and baryon acoustic
oscillations are only observations that distances to a given redshift
are larger than expected from a "dusty" Friedmann–Lemaître universe and
the local measured Hubble constant.
[17]
Supernovae are useful for cosmology because they are excellent
standard candles
across cosmological distances. They allow the expansion history of the
universe to be measured by looking at the relationship between the
distance to an object and its
redshift, which gives how fast it is receding from us. The relationship is roughly linear, according to
Hubble's law.
It is relatively easy to measure redshift, but finding the distance to
an object is more difficult. Usually, astronomers use standard candles:
objects for which the intrinsic brightness, the
absolute magnitude, is known. This allows the object's distance to be measured from its actual observed brightness, or
apparent magnitude.
Type Ia supernovae are the best-known standard candles across
cosmological distances because of their extreme and consistent
luminosity.
Recent observations of supernovae are consistent with a universe made up 71.3% of dark energy and 27.4% of a combination of
dark matter and
baryonic matter.
[18]
Cosmic microwave background
The existence of dark energy, in whatever form, is needed to
reconcile the measured geometry of space with the total amount of matter
in the universe. Measurements of
cosmic microwave background (CMB)
anisotropies indicate that the universe is close to
flat. For the
shape of the universe to be flat, the mass/energy density of the universe must be equal to the
critical density. The total amount of matter in the universe (including
baryons and
dark matter),
as measured from the CMB spectrum, 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%.
[16] The
Wilkinson Microwave Anisotropy Probe (WMAP) spacecraft
seven-year analysis estimated a universe made up of 72.8% dark energy, 22.7% dark matter and 4.5% ordinary matter.
[4] Work done in 2013 based on the
Planck spacecraft
observations of the CMB gave a more accurate estimate of 68.3% of dark
energy, 26.8% of dark matter and 4.9% of ordinary matter.
[20]
Large-scale structure
The theory of
large-scale structure, which governs the formation of structures in the universe (
stars,
quasars,
galaxies and
galaxy groups and clusters), also suggests that the density of matter in the universe is only 30% of the critical density.
A 2011 survey, the WiggleZ galaxy survey of more than 200,000
galaxies, provided further evidence towards the existence of dark
energy, although the exact physics behind it remains unknown.
[21][22] The WiggleZ survey from
Australian Astronomical Observatory scanned the galaxies to determine their redshift. Then, by exploiting the fact that
baryon acoustic oscillations have left
voids
regularly of ~150 Mpc diameter, surrounded by the galaxies, the voids
were used as standard rulers to determine distances to galaxies as far
as 2,000 Mpc (redshift 0.6), which allowed astronomers to determine more
accurately the speeds of the galaxies from their redshift and distance.
The data confirmed
cosmic acceleration up to half of the age of the universe (7 billion years) and constrain its inhomogeneity to 1 part in 10.
[22] This provides a confirmation to cosmic acceleration independent of supernovae.
Late-time integrated Sachs-Wolfe effect
Accelerated cosmic expansion causes
gravitational potential wells and hills to flatten as
photons
pass through them, producing cold spots and hot spots on the CMB
aligned with vast supervoids and superclusters. This so-called late-time
Integrated Sachs–Wolfe effect (ISW) is a direct signal of dark energy in a flat universe.
[23] It was reported at high significance in 2008 by Ho
et al.[24] and Giannantonio
et al.[25]
Observational Hubble constant data
A new approach to test evidence of dark energy through observational
Hubble constant (H(z)) data (OHD) has gained significant attention in recent years.
[26][27][28][29] The Hubble constant is measured as a function of cosmological
redshift.
OHD directly tracks the expansion history of the universe by taking
passively evolving early-type galaxies as “cosmic chronometers”.
[30]
From this point, this approach provides standard clocks in the
universe. The core of this idea is the measurement of the differential
age evolution as a function of redshift of these cosmic chronometers.
Thus, it provides a direct estimate of the Hubble parameter
H(z)=-1/(1+z)dz/dt≈-1/(1+z)Δz/Δt. The merit of this approach is clear:
the reliance on a differential quantity, Δz/Δt, can minimize many common
issues and systematic effects; and as a direct measurement of the
Hubble parameter instead of its integral, like
supernovae and
baryon acoustic oscillations
(BAO), it brings more information and is appealing in computation. For
these reasons, it has been widely used to examine the accelerated cosmic
expansion and study properties of dark energy.
Theories of explanation
Cosmological constant
Lambda, the letter that represents the cosmological constant
The simplest explanation for dark energy is that it is simply the
"cost of having space": that is, a volume of space has some intrinsic,
fundamental energy. This is the cosmological constant, sometimes called
Lambda (hence
Lambda-CDM model) after the Greek letter Λ, the symbol used to represent this quantity mathematically. Since energy and mass are related by
E =
mc2, Einstein's theory of
general relativity predicts that this energy will have a gravitational effect. It is sometimes called a
vacuum energy because it is the energy density of empty
vacuum. In fact, most theories of
particle physics predict
vacuum fluctuations that would give the vacuum this sort of energy. This is related to the
Casimir effect,
in which there is a small suction into regions where virtual particles
are geometrically inhibited from forming (e.g. between plates with tiny
separation). The cosmological constant is estimated by cosmologists to
be on the order of 10
−29 g/cm
3, or about 10
−120 in
reduced Planck units[citation needed]. Particle physics predicts a natural value of 1 in reduced Planck units, leading to a large discrepancy.
The cosmological constant has negative pressure equal to its energy density and so causes the expansion of the universe to
accelerate.
The reason why a cosmological constant has negative pressure can be
seen from classical thermodynamics; Energy must be lost from inside a
container to do work on the container. A change in volume
dV requires work done equal to a change of energy −
P dV, where
P is the pressure. But the amount of energy in a container full of vacuum actually increases when the volume increases (
dV is positive), because the energy is equal to
ρV, where
ρ (rho) is the energy density of the cosmological constant. Therefore,
P is negative and, in fact,
P = −
ρ.
A major outstanding
problem is that most
quantum field theories predict a huge cosmological constant from the energy of the
quantum vacuum, more than 100
orders of magnitude too large.
[8] This would need to be cancelled almost, but not exactly, by an equally large term of the opposite sign. Some
supersymmetric theories require a cosmological constant that is exactly zero,
[31] which does not help because supersymmetry must be broken. The present scientific consensus amounts to
extrapolating the
empirical evidence where it is relevant to predictions, and
fine-tuning
theories until a more elegant solution is found. Technically, this
amounts to checking theories against macroscopic observations.
Unfortunately, as the known error-margin in the constant predicts the
fate of the universe more than its present state, many such "deeper" questions remain unknown.
In spite of its problems, the cosmological constant is in many respects the most
economical solution to the problem of
cosmic acceleration.
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.
Quintessence
In
quintessence models of dark energy, the observed acceleration of the scale factor is caused by the potential energy of a dynamical
field,
referred to as quintessence field. 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, the field must be very light so that it has a large
Compton wavelength.
No evidence of quintessence is yet available, but it has not been
ruled out either. It generally predicts a slightly slower acceleration
of the expansion of the universe than the cosmological constant. Some
scientists 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.
[32] Scalar fields are predicted by the
Standard Model of particle physics and
string theory, but an analogous problem to the cosmological constant problem (or the problem of constructing models of
cosmological inflation) occurs:
renormalization theory predicts that scalar fields should acquire large masses.
The coincidence problem asks why the
acceleration of the Universe began when it did. If 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.
[33]
In 2004, when scientists fit the evolution of dark energy with the
cosmological data, they found that the equation of state had possibly
crossed the cosmological constant boundary (w=−1) from above to below. A
No-Go theorem has been proved that gives this scenario at least two
degrees of freedom as required for dark energy models. This scenario is
so-called
Quintom scenario.
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.
Alternative ideas
Some alternatives to dark energy aim to explain the observational
data by a more refined use of established theories, focusing, for
example, on the gravitational effects of density inhomogeneities, or on
consequences of
electroweak symmetry breaking
in the early universe. If we are located in an emptier-than-average
region of space, the observed cosmic expansion rate could be mistaken
for a variation in time, or acceleration.
[34][35][36][37] A different approach uses a cosmological extension of the
equivalence principle
to show how space might appear to be expanding more rapidly in the
voids surrounding our local cluster. While weak, such effects considered
cumulatively over billions of years could become significant, creating
the illusion of cosmic acceleration, and making it appear as if we live
in a
Hubble bubble.
[38][39][40]
Another class of theories attempts to come up with an
all-encompassing theory of both dark matter and dark energy as a single
phenomenon that modifies the laws of gravity at various scales. An
example of this type of theory is the theory of
dark fluid.
Another class of theories that unifies dark matter and dark energy are
suggested to be covariant theories of modified gravities. These theories
alter the dynamics of the space-time such that the modified dynamic
stems what have been assigned to the presence of dark energy and dark
matter.
[41]
A 2011 paper in the journal
Physical Review D
by Christos Tsagas, a cosmologist at Aristotle University of
Thessaloniki in Greece, argued that it is likely that the accelerated
expansion of the universe is an illusion caused by the relative motion
of us to the rest of the universe. The paper cites data showing that the
2.5 billion ly wide region of space we are inside of is moving very
quickly relative to everything around it. If the theory is confirmed,
then dark energy would not exist (but the "
dark flow" still might).
[42][43]
Some theorists think that dark energy and
cosmic acceleration are a failure of
general relativity on very large scales, larger than
superclusters.
[citation needed] However most attempts at modifying general relativity have turned out to be either equivalent to theories of
quintessence, or inconsistent with observations.
[citation needed] Other ideas for dark energy have come from
string theory,
brane cosmology and the
holographic principle, but have not yet proved
[citation needed] as compelling as quintessence and the cosmological constant.
On string theory, an article in the journal
Nature described:
[44]
- String theories, popular with many particle physicists, make it
possible, even desirable, to think that the observable universe is just
one of 10500 universes in a grander multiverse, says Leonard Susskind,
a cosmologist at Stanford University in California. The vacuum energy
will have different values in different universes, and in many or most
it might indeed be vast. But it must be small in ours because it is only
in such a universe that observers such as ourselves can evolve.
Paul Steinhardt
in the same article criticizes string theory's explanation of dark
energy stating "...Anthropics and randomness don't explain anything... I
am disappointed with what most theorists are willing to accept".
[44]
Another set of proposals is based on the possibility of a double
metric tensor for space-time.
[45][46] It has been argued that time reversed solutions in
general relativity require such double metric for consistency, and that both
dark matter and dark energy can be understood in terms of time reversed solutions of general relativity.
[47]
It has been shown that if
inertia is assumed to be due to the effect of horizons on
Unruh radiation then this predicts galaxy rotation and a cosmic acceleration similar to that observed.
[48]
Variable Dark Energy models
The equation of state of Dark Energy for 4 common models by Redshift.
[49]
A: CPL Model,
B: Jassal Model,
C: Barboza & Alcaniz Model,
D: Wetterich Model
In general, the dark energy can be variable. Modern observational
data have determined the density of dark energy in the present. Using
baryon acoustic oscillations, we can investigate the effect of dark energy in the history of the Universe and we can constrain parameters of the
equation of state
of dark energy. One of the proposed solutions to get closer to
answering the question of dark energy, is to assume that it is variable.
To that end, several models have been proposed. One of their most
popular models is Chevallier–Polarski–Linder model (CPL).
[50][51] Some other common models are, (Barboza & Alcaniz. 2008),
[52] (Jassal et al. 2005),
[53] (Wetterich. 2004).
[54]
Implications for the fate of the universe
Cosmologists estimate that the
acceleration
began 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 decreases 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 have a
line-of-sight velocity that continually increases with time, eventually far exceeding the speed of light.
[55] This is not a violation of
special relativity because the notion of "velocity" used here is different from that of velocity in a local
inertial frame of reference, which is still constrained to be less than the speed of light for any massive object (see
Uses of the proper distance for a discussion of the subtleties of defining any notion of relative velocity in cosmology). Because the
Hubble parameter
is decreasing with time, there can actually be cases where a galaxy
that is receding from us faster than light does manage to emit a signal
which reaches us eventually.
[56][57]
However, because of the accelerating expansion, it is projected that
most galaxies will eventually cross a type of cosmological
event horizon where any light they emit past that point will never be able to reach us at any time in the infinite future
[58]
because the light never reaches a point where its "peculiar velocity"
toward us exceeds the expansion velocity away from us (these two notions
of velocity are also discussed in
Uses of the proper distance). Assuming the dark energy is constant (a
cosmological constant),
the current distance to this cosmological event horizon is about 16
billion light years, meaning that a signal from an event happening
at present
would eventually be able to reach us in the future if the event were
less than 16 billion light years away, but the signal would never reach
us if the event were more than 16 billion light years away.
[57]
As galaxies approach the point of crossing this cosmological event horizon, the light from them will become more and more
redshifted, to the point where the wavelength becomes too large to detect in practice and the galaxies appear to vanish completely
[59][60] (
see Future of an expanding universe). The Earth, the
Milky Way, and the
Virgo Supercluster[contradictory],
however, would remain virtually undisturbed while the rest of the
universe recedes and disappears from view. 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".
[61] Some scenarios, such as the
cyclic model,
suggest this could be the case. It is also possible the universe may
never have an end and continue in its present state forever (see
The Second Law as a law of disorder). While these ideas are not supported by observations, they are not ruled out.
History of discovery and previous speculation
The cosmological constant was first proposed by
Einstein as a mechanism to obtain a solution of the
gravitational field equation that would lead to a static universe, effectively using dark energy to balance gravity.
[62] Not only was the mechanism an inelegant example of
fine-tuning
but it was also later 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
in 1929 showed that the universe appears to be expanding and not static
at all. Einstein reportedly referred to his failure to predict the idea
of a dynamic universe, in contrast to a static universe, as his
greatest blunder.
[63]
Alan Guth and
Alexei Starobinsky proposed in 1980 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 thought 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 thought to be irrelevant to the current
universe.
Nearly all inflation models predict that the total (matter+energy)
density of the universe should be very close to the critical density.
During the 1980s, most cosmological research focused on models with
critical density in matter only, usually 95%
cold dark matter
and 5% ordinary matter (baryons). These models were found to be
successful at forming realistic galaxies and clusters, but some problems
appeared in the late 1980s: notably, the model required a value for the
Hubble constant
lower than preferred by observations, and the model under-predicted
observations of large-scale galaxy clustering. These difficulties became
stronger after the discovery of anisotropy in the
cosmic microwave background by the
COBE spacecraft in 1992, and several modified CDM models came under active study through the mid-1990s: these included the
Lambda-CDM model and a mixed cold/hot dark matter model. The first direct evidence for dark energy came from supernova observations in 1998 of
accelerated expansion in
Riess et al.[11] and in
Perlmutter et al.,
[12]
and the Lambda-CDM model then became the leading model. Soon after,
dark energy was supported by independent observations: in 2000, the
BOOMERanG and
Maxima cosmic microwave background experiments observed the first
acoustic peak in the CMB, showing that the total (matter+energy) density is close to 100% of critical density. Then in 2001, the
2dF Galaxy Redshift Survey
gave strong evidence that the matter density is around 30% of critical.
The large difference between these two supports a smooth component of
dark energy making up the difference. Much more precise measurements
from
WMAP in 2003–2010 have continued to support the standard model and give more accurate measurements of the key parameters.
The term "dark energy", echoing
Fritz Zwicky's "dark matter" from the 1930s, was coined by
Michael Turner in 1998.
[64]
As of 2013, the
Lambda-CDM model is consistent with a series of increasingly rigorous cosmological observations, including the
Planck spacecraft
and the Supernova Legacy Survey. First results from the SNLS reveal
that the average behavior (i.e., equation of state) of dark energy
behaves like Einstein's cosmological constant to a precision of 10%.
[65]
Recent results from the Hubble Space Telescope Higher-Z Team indicate
that dark energy has been present for at least 9 billion years and
during the period preceding cosmic acceleration.
