(Redirected from History of the universe)
This 'timeline of the Big Bang' describes the events that have occurred and will occur according to the
scientific theory of the
Big Bang, using the cosmological time parameter of
comoving coordinates.
Observations suggest that the universe as we know it began around 13.7 billion years ago. Since then, the evolution of the universe has passed through three phases. The very early universe, which is still poorly understood, was the split second in which the universe was so hot that
particles had energies higher than those currently accessible in
particle accelerators on Earth. Therefore, while the basic features of this epoch have been worked out in the big bang theory, the details are largely based on educated guesses.
Following this period, in the early universe, the evolution of the universe proceeded according to known
high energy physics. This is when the first
protons,
electrons and
neutrons formed, then
nuclei and finally
atoms. With the formation of neutral hydrogen, the
cosmic microwave background was emitted.
Finally, the epoch of structure formation began, when matter started to aggregate into the first
stars and
quasars, and ultimately galaxies,
clusters of galaxies and
superclusters formed. The
ultimate fate of the universe is not yet known.
The very early universe
All of our understanding of the very early universe (
cosmogony) is speculative. No accelerator experiments currently probe sufficiently high energies to provide insight into this period. Scenarios differ radically. Some ideas include the
Hartle-Hawking initial state,
string landscape,
brane inflation,
string gas cosmology, and the
ekpyrotic universe. Some of these ideas are mutually compatible, others are not.
Augustinian era
:''Before the Big Bang''
In 1952,
George Gamow, one of the founding fathers of Big Bang cosmology, proposed that before the Big Bang be called the Augustinian era,
[1] after the philosopher
Saint Augustine, who believed time was a property of the Universe that God created and therefore the phrase "before the Creation" would be meaningless as there would be no time for there to be a "before" in. At present it is not known whether or not time in some form did indeed begin with the Big Bang, or indeed anything at all about the moment of creation itself or any kind of "before" - nonetheless the phrase "Augustinian Era" stands as a testament to the fact that the known laws of physics break down in a
Gravitational singularity of a
geometric point at the time
zero of the Big Bang and that before then time as we know it is meaningless.
String theory epoch
Juan Maldacena proved in 1997 that a version of
string theory, with five curled-up dimensions and five large ones, had a surface similar to our four-dimensional universe. The particles in this model resemble
quarks and
gluons. Tests are currently underway to find ways of testing this kind of string theory and
brane inflation. At the
Relativistic Heavy Ion Collider (RHIC) physicists slammed gold nuclei together, producing a temperature 300 million times hotter than the sun, and recreating a
quark-gluon plasma, which rather than behaving like a gas as predicted by
quantum chromodynamics (QCD), behaved like a liquid. It is considered that string theory may explain this finding. According to Maldacena's
holographic conjecture, everything has a counterpart from the ten-dimensional interior onto the fourth dimensional surface. The string theory counterpart equivalent of this quark-gluon plasma is a
black hole [2].
The Planck epoch
:''Up to 10
-43 seconds after the Big Bang''
Main articles: Planck epoch
If
supersymmetry is correct, then during this time the four fundamental forces —
electromagnetism,
weak nuclear force,
strong nuclear force and
gravity — all have the same strength, so they are possibly unified into one fundamental force. Little is known about this epoch, although different theories propose different scenarios. Einstein's theory of
general relativity proposes a
gravitational singularity before this time, but under these conditions the theory is expected to break down due to
quantum effects. Physicists hope that proposed theories of
quantum gravity, such as
string theory and
loop quantum gravity, will eventually lead to a better understanding of this epoch.
The grand unification epoch
:''Between 10
-43 seconds and 10
-35 seconds after the Big Bang''
Main articles: Grand unification epoch
As the universe
expands and cools from the Planck epoch, gravity begins to separate from the fundamental
gauge interactions: electromagnetism and the strong and weak nuclear forces. Physics at this scale may be described by a grand unified theory in which the
gauge group of the
Standard Model is embedded in a much larger group, which is broken to produce the observed forces of nature. Eventually, the grand unification is broken as the strong nuclear force separates from the
electroweak force. This should produce
magnetic monopoles.
The inflationary epoch
:''Between 10
-35 seconds and 10
-32 seconds after the Big Bang''
Main articles: Inflationary epoch
The temperature, and therefore the time, at which cosmic inflation occurs is not known for certain. During inflation, the universe is
flattened and the universe enters a and
isotropic rapidly expanding phase in which the seeds of structure formation are laid down in the form of a primordial spectrum of nearly-
scale-invariant fluctuations. Some energy from photons becomes
virtual quarks and
hyperons, but these particles decay quickly. One scenario suggests that prior to cosmic inflation, the universe was cold and empty, and the immense heat and energy associated with the early stages of the big bang was created through the phase change associated with the end of inflation.
Reheating
During reheating, the exponential expansion that occurred during inflation ceases and the potential energy of the
inflaton field decays into a hot, relativistic
plasma of particles. If grand unification is a feature of our universe, then cosmic inflation must occur during or after the grand unification
symmetry is broken, otherwise magnetic monopoles would be seen in the visible universe. At this point, the universe is dominated by radiation; quarks,
electrons and
neutrinos form.
Baryogenesis
Main articles: Baryogenesis
No known physics can explain the fact that there are so many more
baryons in the universe than
antibaryons. In order for this to be explained, the
Sakharov conditions must be met at some time after inflation. There are hints that this is possible in known physics and from studying grand unified theories, but the full picture is not known.
The early universe
After cosmic inflation ends, the universe is filled with a
quark-gluon plasma. From this point onwards the physics of the early universe is better understood, and less speculative.
The electroweak epoch
:''Between 10
-32 seconds and 10
-12 seconds after the Big Bang''
Main articles: Electroweak epoch
The temperature of the universe is high enough to merge
electromagnetism and the
weak interaction into a single
electroweak interaction. Particle interactions are energetic enough to create large numbers of exotic particles, including
W and Z bosons and
Higgs bosons.
Supersymmetry breaking
Main articles: Supersymmetry breaking
If
supersymmetry is a property of our universe, then it must be broken at an energy as low as 1
TeV, the electroweak symmetry scale. The masses of particles and their
superpartners would then no longer be equal, which could explain why no superpartners of known particles have ever been observed.
The quark epoch
:''Between 10
-12 seconds and 10
-6 seconds after the Big Bang''
Main articles: Quark epoch
In electroweak symmetry breaking, at the end of the electroweak epoch, all the fundamental particles are believed to acquire a mass via the
Higgs mechanism in which the
Higgs boson acquires a
vacuum expectation value. The
fundamental interactions of
gravitation,
electromagnetism, the
strong interaction and the
weak interaction have now taken their present forms, but the temperature of the universe is still too high to allow quarks to bind together to form hadrons.
The hadron epoch
:''Between 10
-6 seconds and 1 second after the Big Bang''
Main articles: Hadron epoch
The quark-gluon plasma which composes the universe cools until
hadrons, including baryons such as
protons and
neutrons, can form. At approximately 1 second after the Big Bang
neutrinos decouple and begin travelling freely through space. This
cosmic neutrino background, while unlikely to ever be observed in detail, is analogous to the
cosmic microwave background that was emitted much later. (See above regarding the quark-gluon plasma, under the String Theory epoch)
The lepton epoch
:''Between 1 second and 3 minutes after the Big Bang''
Main articles: Lepton epoch
The majority of hadrons and anti-hadrons annihilate each other at the end of the hadron epoch, leaving
leptons and anti-leptons dominating the mass of the universe. Approximately 3 seconds after the Big Bang the temperature of the universe falls to the point where new lepton/anti-lepton pairs are no longer created and most leptons and anti-leptons are eliminated in
annihilation reactions, leaving a small residue of leptons.
The photon epoch
:''Between 3 minutes and 380,000 years after the Big Bang''
Main articles: Photon epoch
After most leptons and anti-leptons are annihilated at the end of the lepton epoch the energy of the universe is dominated by
photons. These photons are still interacting frequently with charged protons, electrons and (eventually)
nuclei, and continue to do so for the next 300,000 years.
Nucleosynthesis
:''Between 100 seconds and 300 seconds after the Big Bang''
[3]
Main articles: Big bang nucleosynthesis
During the photon epoch the temperature of the universe falls to the point where atomic nuclei can begin to form. Protons (hydrogen ions) and neutrons begin to combine into atomic nuclei in the process of
nuclear fusion. However, nucleosynthesis only lasts for about three minutes, after which time the temperature and density of the universe has fallen to the point where nuclear fusion cannot continue. At this time, there are about three times more hydrogen ions than helium-4 nuclei and only trace quantities of other nuclei.
Matter domination: 70,000 years
At this time, the densities of non-relativistic matter (atomic nuclei) and relativistic radiation (photons) are equal. The
Jeans length, which determines the smallest structures that can form (due to competition between gravitational attraction and pressure effects), begins to fall and perturbations, instead of being wiped out by
radiation free-streaming, can begin to grow in amplitude.
Recombination: 380,000 years
Hydrogen and helium atoms begin to form and the density of the universe falls. During recombination decoupling occurs, causing the photons to evolve independently from the matter. Most importantly, this means that the photons that compose the
cosmic microwave background are a picture of the universe during this epoch.
WMAP data shows the microwave background radiation variations throughout the Universe from our perspective, though the actual variations are much smoother than the diagram suggests Dark ages
In this epoch, very few atoms are ionized, so the only radiation emitted is the 21 cm spin
line of neutral hydrogen. There is currently an observational effort underway to detect this faint radiation, as it is in principle an even more powerful tool than the cosmic microwave background for studying the early universe.
Structure formation
The Hubble Ultra Deep Fields often showcase galaxies from an ancient era that tell us what the early Stelliferous Age was like. 
Another Hubble image shows an infant galaxy forming nearby, which means this happened very recently on the cosmological timescale. This is evidence that the Universe is not quite finished with galaxy formation yet.
Structure formation in the big bang model proceeds hierarchically, with smaller structures forming before larger ones. The first structures to form are
quasars, which are thought to be bright, early
active galaxies, and
population III stars. Before this epoch, the evolution of the universe could be understood through linear cosmological
perturbation theory: that is, all structures could be understood as small deviations from a perfect homogeneous universe. This is computationally relatively easy to study. At this point non-linear structures begin to form, and the computational problem becomes much more difficult, involving, for example,
N-body simulations with billions of particles.
Reionization
The first quasars form from gravitational collapse. The intense radiation they emit reionizes the surrounding universe. From this point on, most of the universe is composed of
plasma.
Formation of stars
The first stars, most likely
Population III stars, form and start the process of turning the light elements that were formed in the Big Bang (hydrogen, helium and lithium) into heavier elements.
Formation of galaxies
Large volumes of matter collapse to form a galaxy.
Population II stars are formed early on in this process, with
Population I stars formed later.
On July 11, 2007, using the 10 metre Keck II telescope on Mauna Kea, Richard Ellis of the California Institute of Technology at Pasedena and his team found six star forming galaxies about 13.2 billion light years away and therefore created when the universe was only 500 million years old
[4].
Formation of groups, clusters and superclusters
Gravitational attraction pulls galaxies towards each other to form groups, clusters and superclusters.
Formation of our solar system: 8 billion years
Finally, objects on the scale of our solar system form. Our sun is a late-generation star, incorporating the debris from many generations of earlier stars, and formed roughly 5 billion years ago, or roughly 8 to 9 billion years after the big bang.
Today: 13.7 billion years
The best current data estimates the age of the universe today as 13.7 billion years since the big bang. Since the expansion of the universe appears to be accelerating,
superclusters are likely to be the largest structures that will ever form in the universe. The present accelerated expansion prevents any more inflationary structures entering the horizon and prevents new gravitationally bound structures from forming.
Ultimate fate of the universe
As with interpretations of what happened in the very early universe, advances in fundamental physics are required before it will be possible to know the ultimate fate of the universe with any certainty. Below are some of the main possibilities.
Heat death: 1-100 trillion years
This scenario is generally considered to be the most likely, as it occurs if the universe continues expanding as it has been. Over a time scale on the order of a trillion years, existing stars burn out, and the main universe goes dark. The universe approaches a highly entropic state. Over a much longer time scale in the eras following this, galaxies collapse into black holes which subsequently evaporate via
Hawking radiation. In some grand-unification theories, proton decay will convert the remaining interstellar gas into positrons and electrons, which then recombine into photons. In this case, the universe will indefinitely consist solely of a bath of uniform radiation, which is slowly redshifted to lower and lower energy, thus freezing it.
Big crunch: 100 billion years to ?? years
If the energy density of
dark energy were negative or the universe were
closed, then it would be possible that the expansion of the universe would reverse and the universe would contract towards a hot, dense state. This would be analogous to a time-reversal of the
big bang. This is often proposed as part of an
oscillatory universe scenario, such as the
cyclic model. Current observations suggest that this model of the universe is unlikely to be correct, and the expansion will continue.
Big rip
This scenario is possible only if the energy density of
dark energy actually increases without limit over time. Such dark energy is called
phantom energy and is unlike any known kind of energy (except of energy of
virtual particles). In this case, the expansion rate of the universe will increase without limit. Gravitationally bound systems, such as clusters of galaxies, galaxies, and ultimately the solar system will be torn apart. Eventually the expansion will be so rapid as to overcome the electromagnetic forces holding molecules and atoms together. Finally even atomic nuclei will be torn apart and the universe as we know it will end in an unusual kind of
gravitational singularity. In other words, the universe will expand so much that the electromagnetic force holding things together will fall to this expansion, making things fall apart.
Vacuum metastability event
If our universe is in a very long-lived
false vacuum, it is possible that the universe will
tunnel into a lower energy state. If this happens, all structures will be destroyed instantaneously, without any forewarning.
References
1. The Creation of the Universe, Gamow, George, , , Courier Dover Publications, 1961, p. 28 "Thus nothing can be said about the pre-squeeze era of the universe, the era which may be properly called, "St. Augustine's era," since it was St. Augustine of Hippo who first raised the question as to 'what God was doing before He made heaven and earth.'"
2. "New Scientist" July 14th 2007
3. Detailed timeline of Big Bang nucleosynthesis processes
4. "New Scientist" 14th July 2007
External links
★
Holtz, Brian (2002).
Human Knowledge: Foundations and Limits. Retrieved March 25, 2004.
★ PBS Online (2000).
From the Big Bang to the End of the Universe - The Mysteries of Deep Space Timeline. Retrieved March 24, 2005.
★
Schulman, Eric (1997).
The History of the Universe in 200 Words or Less. Retrieved March 24, 2005.
★ Space Telescope Science Institute Office of Public Outreach (2005).
Home of the Hubble Space Telescope. Retrieved March 24, 2005.
★
Fermilab graphics (see "Energy time line from the Big Bang to the present" and "History of the Universe Poster")
★
Astronomers' first detailed hint of what was going on less than a trillionth of a second after time began
★
The Universe Adventure
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