Timeline of the Big Bang
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| Physical Cosmology |
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| Physical Cosmology |
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Universe · Big Bang |
| Early universe |
| Expanding universe |
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Redshift · Hubble's law |
| Structure formation |
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Shape of the universe |
| Components |
| History |
| Cosmology experiments |
| Scientists |
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Einstein · Lemaître · Friedman |
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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, 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 first started to aggregate into the first stars and quasars, and ultimately galaxies, clusters of galaxies and superclusters formed. The future of the universe is not yet firmly known.
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[edit] The very early universe
All 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.
[edit] The Planck epoch
- Up to 10-43 seconds after the Big Bang
If supersymmetry is correct, then at 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 make different predictions. Einstein's theory of general relativity predicts 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 that epoch.
[edit] The Grand unification epoch
- Between 10-43 seconds and 10-35 seconds after the Big Bang
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.
[edit] The inflationary epoch
- Between 10-35seconds and 10-32seconds after the Big Bang
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 homogeneous 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.
[edit] 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.
[edit] 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.
[edit] 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.
[edit] The electroweak epoch
- Between 10-32 seconds and 10-12 seconds after the Big Bang
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.
[edit] 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.
[edit] The quark epoch
- Between 10-12 seconds and 10-6 seconds after the Big Bang
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.
[edit] The hadron epoch
- Between 10-6 seconds and 1 second after the Big Bang
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.
[edit] The lepton epoch
- Between 1 second and 3 seconds after the Big Bang
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 annhilation reactions, leaving a small residue of leptons.
[edit] The photon epoch
- Between 3 seconds and 380,000 years after the Big Bang
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.
[edit] Nucleosynthesis
- Between 100 seconds and 300 seconds after the Big Bang
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.
[edit] 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.
[edit] Recombination: 300,000 years
- See also: Cosmic microwave background
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.
[edit] Dark ages
- See also: 21 centimeter radiation
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.
[edit] Structure formation
- See also: Large-scale structure of the cosmos and Structure formation
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.
[edit] Reionization
- See also: Reionization and 21 centimeter radiation
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.
[edit] Formation of stars
- See also: Star formation
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.
[edit] Formation of galaxies
- See also: Galaxy formation
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.
[edit] Formation of groups, clusters and superclusters
- See also: Large-scale structure of the cosmos
Gravitational attraction pulls galaxies towards each other to form groups, clusters and superclusters.
[edit] Formation of the solar system, 8 billion years
- See also: Solar system
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.
[edit] 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.
[edit] 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.
[edit] Heat death, 1-100 trillion years
- See also: Heat death
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.
[edit] Big Crunch, 100 billion years to ?? years
- See also: Big Crunch
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.
[edit] Big Rip
- See also: 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. 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.
[edit] Vacuum metastability event
- See also: False vacuum
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.
[edit] References
[edit] 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
