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In cosmology, the Big Bang is the scientific theory that describes the early development and shape of the universe. The central idea is that the theory of general relativity can be combined with the observations on the largest scales of galaxies receding from each other to extrapolate the conditions of the universe back or forward in time. A natural consequence of the Big Bang is that in the past the universe had a higher temperature and a higher density. The term "Big Bang" is used both in a narrow sense to refer to a point in time when the observed expansion of the universe (Hubble's law) began, and in a more general sense to refer to the prevailing cosmological paradigm explaining the origin and evolution of the universe.
The term "Big Bang" was coined in 1949 by Fred Hoyle during a BBC radio program, The Nature of Things; the text was published in 1950. Hoyle did not subscribe to the theory and intended to mock the concept.
One consequence of the Big Bang is that the conditions of today's universe are different from the conditions in the past or in the future. From this model, George Gamow in 1948 was able to predict that there should be evidence for a Big Bang in a phenomenon that would later be called the cosmic microwave background radiation (CMB). The CMB was discovered in the 1960s and served as a confirmation of the Big Bang theory over its chief rival, the steady state theory.
According to the Big Bang, 13.7 billion (13.7 × 109) years ago the universe was in an incredibly dense state with huge temperatures and pressures. There is no compelling physical model for the first 10-33 seconds of the universe. Einstein's theory of gravity predicts a gravitational singularity where densities become infinite. To resolve this paradox, a theory of quantum gravity is needed. Understanding this period of the history of the universe is one of the greatest unsolved problems in physics.
History of the theory
In 1927, the Belgian Jesuit priest Georges Lemaître was the first to propose that the universe began with the "explosion" of a "primeval atom". Earlier, in 1918, the Strasbourg astronomer Carl Wilhelm Wirtz had measured a systematic redshift of certain "nebulae", and called this the K-correction; but he wasn't aware of the cosmological implications, nor that the supposed nebulae were actually galaxies outside our own Milky Way.
Albert Einstein's theory of general relativity, developed during this time, admitted no static solutions (that is to say, the universe had to be either expanding or shrinking), a result that he himself considered wrong, and which he tried to fix by adding a cosmological constant. Applying general relativity to cosmology was first done by Alexander Friedmann whose equations describe the Friedmann-Lemaître-Robertson-Walker universe.
In 1929, Edwin Hubble provided an observational basis for Lemaître's theory. Having, in 1913, already determined that most spiral nebulae (what would later be determined to be galaxies) were receding from Earth, Hubble combined this with distance measurements determined by observing Cepheid variable stars in distant galaxies to discover that the galaxies are receding in every direction at speeds (relative to the Earth) directly proportional to their distance. This fact is now known as Hubble's law (see Edwin Hubble: Mariner of the Nebulae by Edward Christianson).
Given the cosmological principle, receding galaxies suggested two opposing possibilities. One, advocated and developed by George Gamow, was that the universe emerged from an extremely hot, dense state a finite time in the past, and has been expanding ever since. The other possibility was Fred Hoyle's steady state model in which new matter would be created as the galaxies moved away from each other. In this model, the universe is roughly the same at any point in time. For a number of years the support for these theories was evenly divided.
In the intervening years, the observational evidence supported the idea that the universe evolved from a hot dense state. Since the discovery of the cosmic microwave background in 1965 it has been regarded as the best theory of the origin and evolution of the cosmos. Before the late 1960s, many cosmologists thought the infinitely dense singularity found in Friedmann's cosmological model was a mathematical over-idealization, and that the universe was contracting before entering the hot dense state and starting to expand again. This is Richard Tolman's oscillating universe. In the sixties, Stephen Hawking and others demonstrated that this idea was unworkable, and the singularity is an essential feature of Einstein's gravity. This led the majority of cosmologists to accept the Big Bang, in which the universe we observe began a finite time ago.
Virtually all theoretical work in cosmology now involves extensions and refinements to the basic Big Bang theory. Much of the current work in cosmology includes understanding how galaxies form in the context of the Big Bang, understanding what happened at the Big Bang, and reconciling observations with the basic theory.
Huge advances in Big Bang cosmology were made in the late 1990s and the early 21st century as a result of major advances in telescope technology in combination with large amounts of satellite data such as that from COBE, the Hubble space telescope and WMAP. These data have allowed cosmologists to calculate many of the parameters of the Big Bang to a new level of precision and led to the unexpected discovery that the expansion of the universe appears to be accelerating.
See also: Timeline of cosmology
Based on measurements of the expansion of the universe using Type Ia supernovae, measurements of the lumpiness of the cosmic microwave background, and measurements of the correlation function of galaxies, the universe has a measured age of 13.7 ± 0.2 billion years. The fact that these three independent measurements are consistent is considered strong evidence for the so-called concordance model that describes the detail nature of the contents of the universe.
The early universe was filled homogeneously and isotropically with a very high energy density. Approximately 10-35 seconds after the Planck epoch, the universe expanded exponentially during a period called cosmic inflation. After inflation stopped, the material components of the universe were in the form of a quark-gluon plasma where the constituent particles were all moving relativistically. By an as yet unknown process, baryogenesis occurred producing the observed asymmetry between matter and antimatter. As the universe grew in size, the temperature dropped, leading to further symmetry breaking processes that manifested themselves as the known forces of physics, elementary particles, and later allowed for the formation of the universe's hydrogen and helium atoms in a process called Big Bang nucleosynthesis. As the universe cooled, matter gradually stopped moving relativistically and its rest mass energy density came to gravitationally dominate over radiation. After about 300,000 years the radiation decoupled from the atoms and continued through space largely unimpeded. This relic radiation is the cosmic microwave background.
Over time, the slightly denser regions of the nearly uniformly distributed matter gravitationally grew into even denser regions, forming gas clouds, stars, galaxies, and the other astronomical structures observable today. The details of this process are dependent on the amount and type of matter in the universe. The three possible types are known as cold dark matter, hot dark matter, and baryonic matter. The best measurements available (from WMAP) show that the dominant form of matter in the universe is in the form of cold dark matter. The other two types of matter make up less than 20% of the matter in the universe.
The universe today appears to be dominated by a mysterious form of energy known as dark energy. Approximately 70% of the total energy density of today's universe is in this form. This component of the universe's composition has the property of causing the expansion of the universe to deviate from a linear velocity-distance relationship by causing spacetime to expand faster than expected at very large distances. Dark energy takes the form of a cosmological constant term in Einstein's field equations of general relativity, but the details of its equation of state and relationship with the standard model of particle physics continue to be investigated both observationally and theoretically.
See also: Timeline of the Big Bang
As it stands today, the Big Bang is dependent on three assumptions:
When first developed, these ideas were simply taken as postulates, but today there are efforts underway to test each of them. The universality of physical laws has been tested to the level that the largest deviation of physical constants over the age of the universe can be is of order 10-5. The isotropy of the universe that defines the Cosmological Principle has been tested to a level of 10-5 and the universe has been measured to be homogenous on the largest scales to the 10% level. There are efforts currently underway to test the Copernican Principle by means of looking at the interaction of clusters of galaxies and the CMB through the Sunyaev-Zeldovich Effect to a level of 1% accuracy.
The Big Bang theory uses Weyl's postulate to unambiguously measure time at any point as the "time since the Planck epoch". Measurements in this system rely on conformal coordinates in which so-called comoving distances and conformal times remove the expansion of the universe from consideration of spacetime measurements. In such a coordinate system, objects moving with the cosmological flow are always the same comoving distance away and the horizon or limit of the universe is set by the conformal time.
The Big Bang is therefore not an explosion of matter moving outward to fill an empty universe; it is spacetime itself that is expanding. It is this expansion that causes the physical distance between any two fixed points in our universe to increase. Objects that are bound together (for example, by gravity) do not expand with spacetime's expansion because the physical laws that govern them are assumed to be uniform and independent of the metric expansion. Moreover, the expansion of the universe on today's local scales is so small that any dependence of physical laws on the expansion is unmeasurable by current techniques.
It is generally stated that there are three observational pillars that support the Big Bang theory of cosmology. These are the Hubble-type expansion seen in the redshifts of galaxies, the detailed measurements of the cosmic microwave background, and the abundance of light elements. Additionally, the observed correlation function of large scale structure in the universe fits well with standard Big Bang theory.
Hubble law expansion
Observations of distant galaxies and quasars show that these objects are redshifted, meaning that the light emitted from them has been proportionately shifted to longer wavelengths. This is seen by taking a spectrum of the objects and then matching the spectroscopic pattern of emission or absorption lines corresponding to atoms of the elements interacting with the radiation. From this analysis, a measured redshift can be determined which is explained by a recessional velocity corresponding to a Doppler shift for the radiation. When the recessional velocities are plotted against the distances to the objects, a linear relationship, known as the Hubble Law, is observed:
v = H0 D
Cosmic microwave background radiation
Main article: Cosmic microwave background radiation
One feature of the Big Bang theory was the prediction of the cosmic microwave background radiation or CMB. As the early universe cooled off due to the expansion, the universe's temperature would fall below 3000 K. Above this temperature, electrons and protons are separate, making the universe opaque to light. Below 3000 K, atoms form, allowing light to pass freely through the gas of the universe. This is known as photon decoupling.
The radiation from this region will travel unimpeded for the remainder of the lifetime of the universe, becoming redshifted because of the Hubble expansion. This results in a redshift of the uniformly distributed blackbody spectrum of the 3000 K to 3 K. It is observed at every point in the universe to come from all directions of space.
In 1964, Arno Penzias and Robert Wilson, while conducting a series of diagnostic observations using a new microwave receiver owned by Bell Laboratories, discovered the cosmic background radiation. Their discovery provided substantial confirmation of the general CMB predictions, and pitched the balance of opinion in favor of the Big Bang hypothesis. Penzias and Wilson were awarded the Nobel Prize for their discovery.
In 1989, NASA launched the Cosmic Background Explorer satellite (COBE), and the initial findings, released in 1990, were consistent with the Big Bang theory's predictions regarding CMB, finding a local residual temperature of 2.726 K and determining that the CMB was isotropic to an accuracy of 10-5. During the 1990s, CMB data was studied further to see if small anisotropies predicted by the Big Bang theory would be observed. They were found in 2000 by the Boomerang experiment.
In early 2003 the results of the Wilkinson Microwave Anisotropy satellite (WMAP) were analyzed, giving the most accurate cosmological values we have to date. This satellite also disproved several specific inflationary models, but the results were consistent with the inflation theory in general.
Abundance of primordial elements
Main article: Big Bang nucleosynthesis
Using the Big Bang model it is possible to calculate the concentration of helium-4, helium-3, deuterium and lithium-7 in the universe. All the abundances depend on a single parameter, the ratio of photons to baryons. The abundances predicted are about 25 percent for 4He, a 2H/H ratio of about 10-3, a 3He/H of about 10-4 and a 7Li/H abundance of about 10-9.
Measurements of primordial abundances for all four isotopes are consistent with a unique value of that parameter and the fact that the measured abundances are in the same range as the predicted ones is considered strong evidence for the Big Bang. There is no obvious reason outside of the Big Bang that, for example, the universe should have more helium than deuterium or more deuterium than 3He.
Galactic evolution and quasar distribution
The details of the distribution of galaxies and quasars are both constraints and confirmations of current theory. The finite age of the universe at earlier times means that galaxy evolution is closely tied to the cosmology of the universe. The types and distribution of galaxies appears to change markedly over time, evolving by means of the Boltzmann Equation. Observations reveal a time-dependent relationship of the galaxy and quasar distributions, star formation histories, and the type and size of the largest-scale structures in the universe (superclusters). These observations are in statistical agreement with simulations. They are well explained by the Big Bang theory and help constrain model parameters.
Historically, a number of problems have arisen within the Big Bang theory. Some of them are today mainly of historical interest, and have been avoided either through modifications to the theory or as the result of better observations. Other issues, such as the cuspy halo problem and the dwarf galaxy problem of cold dark matter, are not considered to be fatal as they can be addressed through refinements of the theory. Some detractors of the Big Bang cite these problems as ad hoc modifications and addenda to the theory. Most often attacked are the parts of standard cosmology that include dark matter, dark energy, and cosmic inflation. These are strongly suggested by observations of the cosmic microwave background, large scale structure and type IA supernovae, but remain at the frontiers of inquiry in physics. There is not yet a consensus on the particle physics origin of dark matter, dark energy and inflation. While their gravitational effects are understood observationally and theoretically, they have not yet been incorporated into the standard model of particle physics in an accepted way.
There are a small number of proponents of non-standard cosmologies who believe that there was no Big Bang at all. While some aspects of standard cosmology are inadequately explained in the standard model, most physicists accept that the close agreement between Big Bang theory and observation have firmly established all the basic parts of the theory.
What follows is a short list of standard Big Bang "problems" and puzzles:
The horizon problem
The horizon problem results from the premise that information cannot travel faster than light, and hence two regions of space which are separated by a greater distance than the speed of light multiplied by the age of the universe cannot be in causal contact. The observed isotropy of the cosmic microwave background (CMB) is problematic in this regard, because the horizon size at that time corresponds to a size that is about 2 degrees on the sky. If the universe has had the same expansion history since the Planck epoch, there is no mechanism to allow for these regions to have the same temperature.
This apparent inconsistency is resolved by inflationary theory in which a homogeneous and isotropic scalar energy field dominates the universe at a time 10-35 seconds after the Planck epoch. During inflation, the universe undergoes exponential expansion, and regions in causal contact expand past each other's horizons. Heisenberg's uncertainty principle predicts that there would be quantum thermal fluctuations during the inflationary phase, which would be magnified to cosmic scale. These fluctuations serve as the seeds of all current structure in the universe. After inflation, the universe expands by means of a Hubble Law, and regions that were out of causal contact come back into the horizon. This explains the observed isotropy of the CMB. Inflation predicted that the primordial fluctuations are nearly scale invariant and Gaussian which has been accurately confirmed by measurements of the CMB.
The flatness problem is an observational problem that results from considerations of the geometry associated with Friedmann-Lemaître-Robertson-Walker metric. In general, the universe can have three different kinds of geometries: hyperbolic geometry, Euclidean geometry, or elliptic geometry. Each one of these geometries is tied directly to the critical density of the universe, the hyperbolic corresponding to less than the critical density, elliptic corresponding to greater than the critical density, and Euclidean corresponding to exactly equal to the critical density. The universe is measured to be required to be within one part in 1015 of the critical density in its earliest stages. Any deviation more than that would have caused either a Heat Death or a Big Crunch and the universe would not exist as it does today.
The resolution to this problem is again offered by inflationary theory. During the inflationary period, spacetime expanded to such an extent that any residual curvature associated with it would have been completely smoothed out to a high degree of precision. Thus, the universe is driven to be flat by inflation.
The magnetic monopole problem was an objection that was raised in the late 1970s. Grand unification theories predicted point defects in space that would manifest as magnetic monopoles, and the density of these monopoles was much higher than what could be accounted for. This problem is also resolvable by the addition of cosmic inflation which removes all point defects from the observable universe in the same way that the geometry is driven to flatness.
During the 1970s and 1980s various observations (notably of galactic rotation curves) showed that there was not sufficient visible matter in the universe to account for the apparent strength of gravitational forces within and between galaxies. This led to the idea that up to 90% of the matter in the universe is non-baryonic dark matter. In addition, assuming that the universe was mostly normal matter led to predictions that were strongly inconsistent with observations. In particular, the universe is far less lumpy and contains far less deuterium than can be accounted for without dark matter. While dark matter was initially controversial, it is now a widely accepted part of standard cosmology due to observations in the anisotropies in the CMB, galaxy cluster velocity dispersions, large scale structure distributions, gravitational lensing studies, and x-ray measurements from galaxy clusters. Dark matter particles have only been detected through their gravitational signatures, and have not yet been observed in laboratories. However, there are many particle physics candidates for dark matter, and several projects to detect them are underway.
In the 1990s, detailed measurements of the mass density of the universe revealed a value that was 30% that of the critical density. For the universe to be flat, as is indicated by measurements of the cosmic microwave background, this would have meant that fully 70% of the energy density of the universe was left unaccounted for. Measurements of Type Ia supernovae reveal that the universe is undergoing a non-linear acceleration of the Hubble Law expansion of the universe. General relativity requires that this additional 70% be made up by an energy component with large negative pressure. The nature of the so-called dark energy remains one of the great mysteries of the Big Bang. Possible candidates include a scalar cosmological constant and quintessence. Observations to help understand this are ongoing.
Globular cluster age
A certain set of observations were made in the mid-1990s involving the ages of globular clusters that were found to be inconsistent with the Big Bang. Computer simulations that matched the observations of the stellar populations of globular clusters suggested that they were about 15 billion years old, which conflicted with the 13.7 billion year age of the universe. This issue was generally resolved in the late 1990s with other new computer simulations which included the effects of mass loss due to stellar winds indicated a much younger age for globular clusters. There still remain some questions as to how accurately the ages of the clusters are measured, but it is clear that these objects are some of the oldest in the universe.
The future according to the Big Bang theory
In the past, before observations of dark energy, cosmologists considered two scenarios for the future of the universe. If the mass density of the universe is above the critical density, then the universe would reach a maximum size and begin to collapse in a Big Crunch. In this scenario, the universe would become denser and hotter again, ending with a state that was similar to that in which it started. Alternatively, if the mass density in the universe were equal to or below the critical density, the expansion would slow down, but never stop. New star formation would cease as the universe grows less dense. The average temperature of the Universe would asymptotically approach absolute zero. Black holes would evaporate. The entropy of the universe would increase to the point where no organized form of energy could be extracted from it, a scenario also known as heat death. Moreover, if proton decay exists, then hydrogen, the predominant form of baryonic matter in the universe today, would disappear, leaving only radiation.
Modern observations of accelerated expansion have led cosmologists to the Lambda-CDM model of the universe. This model contains dark energy, in the form of a cosmological constant. This energy causes more and more of the presently visible universe to pass beyond our horizon and out of contact with us. It is not known what will happen after this. The cosmological constant theory suggests that only gravitationally bound systems, such as galaxies, would remain together, and they too would be subject to heat death, as the universe cools and expands. Other so-called phantom energy theories suggest that ultimately galaxy clusters and eventually galaxies themselves will be torn apart by the ever increasing expansion in a so-called Big Rip.
See also Ultimate fate of the universe.
Speculative physics beyond the Big Bang
There remains the possibility that the Big Bang will be developed in the future and in particular, we might learn something about inflation or whatever came immediately before the Big Bang. It might be the case that there are parts of the universe well beyond what can be observed in principle. In the case of inflation this is required: exponential expansion has pushed large regions of space beyond our observable horizon. It may be possible to deduce what happened when we better understand physics at very high energy scales. Speculations about this tend to involve theories of quantum gravity.
Some proposals are:
- chaotic inflation
- brane cosmology models, including the ekpyrotic model in which the Big Bang is the result of a collision between branes
- oscillatory universe which holds that the early universe's hot, dense state matches on to a contracting universe similar to ours. This yields a universe with an infinite number of big bangs and big crunches. The cyclic extension of the ekpyrotic model is a modern version of such a scenario.
- models including the Hartle-Hawking boundary condition in which the whole of space-time is finite
Some of these scenarios are qualitatively compatible with one another. Each involves untested hypotheses.
Philosophical and religious interpretations
Philosophically, there are a number of interpretations of the Big Bang theory that are entirely speculative or extra-scientific. Some of these ideas purport to explain the cause of the Big Bang itself (first cause), and have been criticized by some naturalist philosophers as being modern creation myths. Some people believe that the Big Bang theory lends support to traditional views of creation, for example as given in Genesis, while others believe that all Big Bang theories are inconsistent with such views.
The Big Bang as a scientific theory is not associated with any religion. While certain fundamentalist interpretations of religions conflict with the history of the universe as put forth by the Big Bang, there are also more liberal interpretations that do not.
The following is a list of various religious interpretations of the Big Bang theory:
- A number of Christian apologists, and the Roman Catholic Church in particular, have accepted the Big Bang as a description of the origin of the universe, interpreting it to allow for a philosophical first cause.
- Students of Kabbalah, deism and other non-anthropomorphic faiths concord with the Big Bang theory, notably the theory of "divine retraction" (Tzimtzum), as explained by Jewish Scholar Moses Maimonides. Similarly, Pandeists, who believe that an initially sentient God designed and then transformed himself into the non-sentient universe, often identify the Big Bang as the moment of transformation.
- Some modern Islamic scholars believe that the Qur'an parallels the Big Bang in its account of creation, described as follows: "the heavens and the earth were joined together as one unit, before We clove them asunder" (21:30). The Qur'an also appears to describe an expanding universe: "The heavens, We have built them with power. And verily, We are expanding it" (51:47).
- Certain theistic branches of Hinduism, such as the Vaishnava-traditions, conceive of a theory of creation with similarities to the theory of the Big Bang. The Hindu-mythos, narrated for example in the third book of the Bhagavata Purana (primarily, chapters 10 and 26), describes a primordial state which bursts forth as the Great Vishnu glances over it, transforming into the active state of the sum-total of matter ("prakriti").
- Buddhism has a concept of a universe that has no creation event per se. The Big Bang, however, is not seen to be in conflict with this since there are ways to get an eternal universe within the paradigm. A number of popular Zen philosophers were intrigued, in particular, by the concept of the oscillating universe.
- The future according to Big Bang theory
- Cosmology, astrophysics and astronomy
- A Brief History of Time
- Magnitude order
- Primordial black hole
- Stellar population
- Theoretical astrophysics
- History of astronomy
- Supermassive black hole
- Physics topics
- Cosmic microwave background radiation
- Timeline of cosmic microwave background astronomy
- Blackbody spectrum
- Cosmic variance
- Integrated Sachs Wolfe effect
- Spherical harmonics
- Sachs-Wolfe effect
- Observational experiments
- Hubble Space Telescope
- Cosmic Background Explorer (COBE)
- Far Ultraviolet Spectroscopic Explorer (FUSE)
- Gamma-ray Large Area Space Telescope
- Wilkinson Microwave Anisotropy Probe (WMAP)
- Atomic chemical elements
- List of astronomical topics
- List of famous experiments
- List of time periods
- Timeline of the Universe
- Big Bang used in other Fiction
External links and references
Big Bang overviews
- LaRocco, Chris and Blair Rothstein, "THE BIG BANG: It sure was BIG!!".
- Open Directory Project: Cosmology
- PBS.org, "From the Big Bang to the End of the Universe. The Mysteries of Deep Space Timeline"
- "Welcome to the History of the Universe". Penny Press Ltd.
- Shestople, Paul, "Big Bang Primer".
- Wright, Edward L., "Brief History of the Universe".
Beyond the Big Bang
- Cambridge University Cosmology, "The Hot Big Bang Model".
- Smithsonian Institution, "UNIVERSE! - The Big Bang and what came before".
- Whitehouse, David, "Before the Big Bang". BBC News. April 10, 2001.
- D'Agnese, Joseph, "The last Big Bang man left standing, physicist Ralph Alpher devised Big Bang Theory of universe". Discover, July, 1999.
- Felder, Gary, "The Expanding Universe".
- Links to sample text and reviews: Big Bang by Simon Singh
- John C Mather and John Boslough 1996, The very first light : the true inside story of the scientific journey back to the dawn of the universe. ISBN 0-465-01575-1 p.300: LeMaitre, Annals of the Scientific Society of Brussels 47A (1927):41 - GRT implies universe had to be expanding. But Einstein brushed him off in the same year. LeMaitre's note was translated in Monthly Notice of the Royal Astronomical Society (1931):483-490.
- See also LeMaitre, Nature 128(1931) suppl.:704. with a reference to the primeval atom.
- See review article by Ralph Alpher and Robert Herman Physics Today Aug 1988 pp24-34 which references
- Alpher 1948 Phys Rev D 74,1737
- Alpher and Herman 1948 Phys Rev D 74,1577
- Alpher Herman and Gamow 1948 Nature 162,774
Most scientific papers about cosmology are initially released as preprints on arxiv.org. They are generally quite technical, but sometimes have introductions in plain English. The most relevant archives, which cover experiment and theory, are the astrophysics archive, where papers closely grounded in observations are released, and the general relativity and quantum cosmology archive, which covers more speculative ground. Papers of interest to cosmologists also frequently appear on the high energy phenomenology and high energy theory archives.
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