- Cosmic inflation
In

physical cosmology ,**cosmic inflation**is the idea that theuniverse passed through a phase of exponential expansion that was driven by a negative-pressurevacuum energy density. [*Liddle and Lyth (2000) and Mukhanov (2005) are recent cosmology textbooks with extensive discussions of inflation. Kolb and Turner (1988) and Linde (1990) miss some recent developments, but are still widely used. Peebles (1993) provides a technical discussion with historical context. Recent review articles are Lyth and Riotto (1999) and Linde (2005). Guth (1997) and Hawking (1998) give popular introductions to inflation with historical remarks.*]As a direct consequence of this expansion, all of the observable universe originated in a small causally-connected region. Inflation answers the classic conundrum of the

big bang cosmology: why does the universe appear flat,homogeneous andisotropic in accordance with thecosmological principle when one would expect, on the basis of the physics of the big bang, a highly curved, inhomogeneous universe? Inflation also explains the origin of thelarge-scale structure of the cosmos .Quantum fluctuation s in the microscopic inflationary region, magnified to cosmic size, become the seeds for the growth of structure in the universe (seegalaxy formation and evolution andstructure formation ).Inflation was proposed in January, 1980 by

Alan Guth SLAC seminar, "10-35 seconds after the Big Bang", 23rd January, 1980. see Guth (1997), pg 186] A. H. Guth, "The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems", "Phys. Rev. D"**23**, 347 (1981).] and was given its modern form independently byAndrei Linde ,A. Linde, "A New Inflationary Universe Scenario: A Possible Solution Of The Horizon, Flatness, Homogeneity, Isotropy And Primordial Monopole Problems", "Phys. Lett. B"**108**, 389 (1982).] and byAndreas Albrecht andPaul Steinhardt .A. Albrecht and P. J. Steinhardt, "Cosmology For Grand Unified Theories With Radiatively Induced Symmetry Breaking," "Phys. Rev. Lett."**48**, 1220 (1982).]While the detailed

particle physics mechanism responsible for inflation is not known, the basic picture makes a number of predictions that have been confirmed by observational tests. Inflation is thus now considered part of the standard hotbig bang cosmology. The hypothetical particle or field thought to be responsible for inflation is called the.inflaton **Overview**Inflation suggests that there was a period of exponential expansion in the very early universe. Because in a fast expanding universe, the distance to the

cosmological horizon is constant, it is not clear whether such a universe should be called "small" or "large". If the philosophical definition of the universe is restricted to be theobservable universe , an inflating universe is small, and only becomes large once inflation has ended and the cosmological horizon is free to expand. If the philosophical position is that the universe is mostly unobservable, then the unobservable portion is expanding exponentially.**pace expands**To say that space expands exponentially means that two

inertial observer s are drawn further apart with time. In stationary coordinates for one observer, a patch of an inflating universe has the following polar metric::$ds^2\; =\; -\; (1-\; Lambda\; r^2)\; dt^2\; +\; \{1over\; 1-Lambda\; r^2\}\; dr^2\; +\; r^2\; dOmega$This is just like an inside-outblack hole metric — it has a zero in the dt component on a fixed radius sphere called thecosmological horizon . Objects are drawn away from the observer at r=0 towards the cosmological horizon, leading them to fall in after a finite proper time. This means that any inhomogeneities are smoothed out, just as any bumps or matter on the surface of a black hole horizon are swallowed and disappear.Since the space time metric has no explicit time dependence, once an observer has fallen onto the cosmological horizon, observers closer in take its place. This process of falling outward and replacement points closer in are always steadily replacing points further out — an exponential expansion of space-time.

This steady-state exponentially expanding spacetime is called a

de Sitter space , and to sustain it there must be acosmological constant , a vacuum energy proportional to $Lambda$ everywhere. The physical conditions from one moment to the next are stable: the rate of expansion, called theHubble parameter , is nearly constant. Inflation is often called a period of "accelerated expansion" because the distance between two fixed observers is increasing at an accelerating rate as they move apart. (but $Lambda$ can stay approximately constant seedeceleration parameter .)**Few inhomogeneities remain**Cosmic inflation has the important effect of smoothing out inhomogeneities, anisotropies and the curvature of space. This pushes the universe into a very simple state, in which it is completely dominated by the

inflaton field, the source of the cosmological constant, and the only significant inhomogeneities are the tiny quantum fluctuations in theinflaton . Inflation also dilutes exotic heavy particles, such as themagnetic monopole s predicted by many extensions to theStandard Model ofparticle physics . If the universe was only hot enough to form such particles "before" a period of inflation, they would not be observed in nature, as they would be so rare that it is quite likely that there are none in theObservable universe . Together, these effects are called the inflationary "no-hair theorem" [*Kolb and Turner (1988).*] by analogy with theno hair theorem forblack hole s.The "no-hair" theorem works essentially because the cosmological horizon is no different from a black-hole horizon except for philosophical disagreements about what is on the other side. In terms of the unobservable universe, the interpretation of the no-hair theorem is that the unobservable universe expands by an enormous factor during inflation. In an expanding universe, energy densities generally fall as the volume of the universe increases. For example, the density of ordinary "cold" matter (dust) goes as the inverse of the volume: when linear dimensions double, the energy density goes down by a factor of eight. The energy density in radiation goes down even more rapidly as the universe expands. When linear dimensions are doubled, the energy density in radiation falls by a factor of sixteen.During inflation, the energy density in the

inflaton field is roughly constant. However, the energy density in inhomogeneities, curvature, anisotropies and exotic particles is falling, and through sufficient inflation these become negligible. This leaves an empty, flat, and symmetric universe, which is filled with radiation when inflation ends.**Key requirement**A key requirement is that inflation must continue long enough to produce the present observable universe from a single, small inflationary

Hubble volume . This is necessary to ensure that the universe appears flat, homogeneous and isotropic at the largest observable scales. This requirement is generally thought to be satisfied if the universe expanded by a factor of at least 10^{26}during inflation. [*This is usually quoted as 60 "e"-folds of expansion, where "e"*]^{60}≈ 10^{26}. It is equal to the amount of expansion since reheating, which is roughly "E"_{inflation}/"T"_{0}, where T_{0}= 2.7 K is the temperature of the cosmic microwave background today. See, "e.g." Kolb and Turner (1998) or Liddle and Lyth (2000).**Reheating**At the end of inflation, a process called "reheating" occurs, in which the

inflaton particles decay into the radiation that starts the hot big bang. It is not known how long inflation lasted but it is usually thought to be extremely short compared to the age of the universe.**Motivation**Inflation resolves several problems in the

Big Bang cosmology that were pointed out in the 1970s. [*Much of the historical context is explained in chapters 15–17 of Peebles (1993).*] These problems arise from the observation that to look like it does "today," the universe would have to have started from very finely tuned, or "special" initial conditions at the Big Bang. Inflation attempts to resolve these problems by providing a dynamical mechanism that drives the universe to this special state, thus making a universe like ours much more likely in the context of the Big Bang theory.**Horizon problem**The

horizon problem [*cite journal|title=The isotropy of the universe | doi = 10.1088/0264-9381/15/2/008 |first=Charles W.|last=Misner|year=1968|journal=Astrophysical Journal|volume=151|pages=431*] cite book | last = Misner | first = Charles | coauthors = Thorne, Kip S. and Wheeler, John Archibald | title = Gravitation | location = San Francisco | publisher = W. H. Freeman | year = 1973 | isbn = 0-7167-0344-0|pages=pp. 489–490, 525–526] cite book | first = Steven | last = Weinberg | title = Gravitation and Cosmology | publisher = John Wiley | year = 1971 | isbn = 0-471-92567-5|pages=pp. 740, 815] is the problem of determining why the universe appears statistically homogeneous and isotropic in accordance with thecosmological principle . For example, molecules in a canister of gas are distributed homogeneously and isotropically because they are in thermal equilibrium: gas throughout the canister has had enough time to interact to dissipate inhomogeneities and anisotropies. The situation is quite different in the big bang model without inflation, because gravitational expansion does not give the early universe enough time to equilibrate. In a big bang with only thematter andradiation known in theStandard Model , two widely separated regions of the observable universe cannot have equilibrated because they move apart from each other faster than thespeed of light — thus have never come in tocausal contact : in the history of the universe, back to the earliest times, it has not been possible to send a light signal between the two regions. Because they have no interaction, it is difficult to explain why they have the same temperature (are thermally equilibrated). This is because theHubble radius in a radiation or matter-dominated universe expands much more quickly than physical lengths and so points that are out of communication are coming into communication. Historically, two proposed solutions were thePhoenix universe ofGeorges Lemaître [*cite journal|last=Lemaître|first=Georges|title=The expanding universe|journal=Ann. Soc. Sci. Bruxelles|volume=47A|pages=49|year=1933, English in "Gen. Rel. Grav."*] and the related**29**:641-680, 1997.oscillatory universe ofRichard Chase Tolman , [*cite book | author=R. C. Tolman | title= Relativity, Thermodynamics, and Cosmology | location=Oxford | publisher=Clarendon Press | year=1934 | id=LCCN 340-32023 Reissued (1987) New York: Dover ISBN 0-486-65383-8.*] and theMixmaster universe ofCharles Misner . [*cite journal|title=Mixmaster universe | doi = 10.1088/1751-8113/41/15/155201 |first=Charles W.|last=Misner|year=1969|journal=Phys. Rev. Lett.|volume=22|pages=1071–74*] Lemaître and Tolman proposed that a universe undergoing a number of cycles of contraction and expansion could come into thermal equilibrium. Their models failed, however, because of the buildup ofentropy over several cycles. Misner made the (ultimately incorrect) conjecture that the Mixmaster mechanism, which made the universe "more" chaotic, could lead to statistical homogeneity and isotropy.**Flatness problem**Another problem is the

flatness problem (which is sometimes called one of theDicke coincidences, with the other being thecosmological constant problem ). [*cite book|last=Dicke |first=Robert H.|title=Gravitation and the Universe |location = Philadelphia | publisher=American Philosopical Society | year = 1970*] [*cite conference|title=The big bang cosmology – enigmas and nostrums|first=Robert H.|last=Dicke|coauthors=P. J. E. Peebles | year = 1979| booktitle = General Relativity: an Einstein Centenary Survey|editor=ed. S. W. Hawking and W. Israel | publisher = Cambridge University Press*] It had been known in the 1960sFact|date=February 2007 that the density of matter in the universe was comparable to thecritical density necessary for a flat universe (that is, a universe whose large scalegeometry is the usualEuclidean geometry , rather than a non-Euclidean hyperbolic orspherical geometry ).Therefore, regardless of the

shape of the universe the contribution of spatial curvature to the expansion of the universe could not be much greater than the contribution of matter. But as the universe expands, the curvatureredshift s away more slowly than matter and radiation. Extrapolated into the past, this presents afine-tuning problem because the contribution of curvature to the universe must be exponentially small (sixteen orders of magnitude less than the density of radiation atbig bang nucleosynthesis , for example). This problem is exacerbated by recent observations of the cosmic microwave background that have demonstrated that the universe is flat to the accuracy of a few percent.Fact|date=January 2008**Magnetic monopole problem**The

magnetic monopole problem (sometimes called the exotic relics problem) is a problem that suggests that if the early universe were very hot, a large number of very heavy, stablemagnetic monopole s would be produced. This was a problem with Grand Unified Theories, popular in the 1970s and 1980s, which proposed that at high temperatures (such as in the early universe) theelectromagnetic force , strong and weaknuclear force s are not actually fundamental forces but arise due tospontaneous symmetry breaking from a much simplergauge theory . [*The importance of grand unification has waned somewhat since the early 1990s, as the simplest theories have been ruled out by*] These theories predict a number of heavy, stable particles which have not yet been observed in nature. The most notorious is the magnetic monopole, a kind of stable, heavy "knot" in the magnetic field. [proton decay experiments. However, many people still believe that a supersymmetric Grand Unified Theory is built intostring theory , so it is still seen as a triumph for inflation that it is able to deal with these relics. See, "e.g." Kolb and Turner (1988) and cite conference|title=Grand Unified Theories|first=Stuart|last=Raby|url=http://arxiv.org/abs/hep-ph/0608183|booktitle=Galapagos World Summit on Physics Beyond the Standard Model|editor=ed. Bruce Hoeneisen|year=2006*cite journal|last='t Hooft|first=Gerard|title=Magnetic monopoles in Unified Gauge Theories|journal=Nucl. Phys.|volume=B79|pages=276–84|year=1974*] [*cite journal|first=Alexander M.|last=Polyakov|title=Particle spectrum in quantum field theory|journal=JETP Lett.|volume=20|pages=194–5|year=1974*] Monopoles are expected to be copiously produced in Grand Unified Theories at high temperature, and they should have persisted to the present day. [*cite journal|title=On the concentration of relic monopoles in the universe|first=Ya.|last=Zel'dovich|coauthros=M. Yu. Khlopov|year=1978|journal=Phys. Lett.|volume=B79|pages=239–41*] [*cite journal|title=Cosmological production of superheavy magnetic monopoles | doi = 10.1103/PhysRevLett.43.1365 |year=1979|journal=Phys. Rev. Lett.|volume=43|pages=1365|first=John|last=Preskill*] To very high precision, magnetic monopoles have been shown not to exist in nature, [*See, "e.g." cite journal|last=Yao|first=W.–M.|coauthors="et al." (*] whereas according to the big bang theory (without cosmic inflation) they should have been copiously produced in the hot, dense early universe and since become the primary constituent of the universe.Particle Data Group )|title=Review of Particle Physics | doi = 10.1088/0954-3899/33/1/001 |journal=J. Phys.|volume=G33|pages=1|url=http://pdg.lbl.gov/|authorlink=Particle Data Group|unused_data=|date2006**History****Precursors**In the early days of

General Relativity ,Albert Einstein introduced thecosmological constant to allow a static solution which was a three dimensional sphere with a uniform density of matter. A little later,Willem de Sitter found a highly symmetric inflating universe, which described a universe with a cosmological constant which is otherwise empty. [*cite journal|first=Willem|last=de Sitter|title=Einstein's theory of gravitation and its astronomical consequences. Third paper|journal=Monthly Notices of the Royal Astronomical Society|volume=78|pages=3–28|year=1917*] Einstein's solution is unstable, and if there are small fluctuations, it eventually turns into de Sitter's.In the early 1970s

Zeldovich noticed the serious flatness and horizon problems of big bang cosmology; before his work, cosmology was presumed to be symmetrical on purely philosophical grounds. In the Soviet Union, this and other considerations ledBelinski andKhalatnikov to formulate themixmaster universe , an analysis of the chaos near a singularity in General Relativity. Starobinsky formulated an early chaotic version of inflation in 1979 [*Starobinsky, A. A. - Spectrum Of Relict Gravitational Radiation And The Early State Of The Universe - JETP Lett. 30, 682 (1979) {Pisma Zh. Eksp. Teor. Fiz. 30, 719 (1979)}.*] , which was advanced byVilenkin and Starobinsky. While this was not as transparent a solution to the cosmological problems as Guth's, it remains a possibility. In the late 1970s,Sidney Coleman applied theinstanton techniques developed byAlexander Polyakov and collaborators to study the fate of thefalse vacuum in quantum field theory. Like a metastable phase in statistical mechanics--- water below the freezing temperature or above the boiling point--- a quantum field would need to nucleate a large enough bubble of the new vacuum, the new phase, in order to make a transition. Coleman found the most likely decay pathway for vacuum decay and calculated the inverse lifetime per unit volume. He eventually noted that gravitational effects would be significant, but he did not calculate these effects and did not apply the results to cosmology.In 1978, Zeldovich noted the monopole problem, which was an unambiguous quantitative version of the horizon problem, this time in a fashionable subfield of particle physics, which led to several speculative attempts to resolve it. In 1980, working in the west,

Alan Guth realized that false vacuum decay in the early universe would solve the problem.**Guth, Starobinsky and others**Inflation was proposed in January, 1980 by

Alan Guth as a mechanism for resolving these problems. Contemporary with Guth,Alexei Starobinsky argued that quantum corrections to gravity would replace the initial singularity of the universe with an exponentially expanding state. [*cite journal|first=Alexei A.|last=Starobinsky|title=A new type of isotropic cosmological models without singularity|journal=Phys. Lett.|volume=B91|pages=99–102|year=1980*]Demosthenes Kazanas anticipated part of Guth's work by suggesting that exponential expansion could eliminate theparticle horizon and perhaps solve the horizon problem, [*cite journal|first=D.|last=Kazanas|title=Dynamics of the universe and spontaneous symmetry breaking|journal=Astrophys. J.|volume=241|pages=L59–63|year=1980|doi=10.1086/183361*] and Sato suggesting that an exponential expansion could eliminatedomain wall s (another kind of exotic relic). [*cite journal|first=K.|last=Sato|title=Cosmological baryon number domain structure and the first order phase transition of a vacuum|journal=Phys. Lett.|volume=B33|pages=66–70|year=1981*]**Guth**Guth was the first to assemble a complete picture of how all these initial conditions problems could be solved by an exponentially expanding state.

Guth proposed that as the early universe cooled, it was trapped in a

false vacuum with a high energy density, which is much like acosmological constant . As the very early universe cooled it was trapped in a metastable state (it was supercooled) which it could only decay out of through the process of bubble nucleation viaquantum tunneling . Bubbles of true vacuum spontaneously form in the sea of false vacuum and rapidly begin expanding at thespeed of light . Guth recognized that this model was problematic because the model did not reheat properly: when the bubbles nucleated, they did not generate any radiation. Radiation could only be generated in collisions between bubble walls. But if inflation lasted long enough to solve the initial conditions problems, collisions between bubbles became exceedingly rare. In any one causal patch, it is likely that only one bubble will nucleate.**Linde, Albrecht and Steinhardt**The bubble collision problem was solved by

Andrei Linde and independently byAndreas Albrecht andPaul Steinhardt in a model named "new inflation" or "slow-roll inflation" (Guth's model then became known as "old inflation"). In this model, instead of tunneling out of a false vacuum state, inflation occurred by ascalar field rolling down a potential energy hill. When the field rolls very slowly compared to the expansion of the universe, inflation occurs. However, when the hill becomes steeper, inflation ends and reheating can occur.**Effects of asymmetries**Eventually, it was shown that new inflation does not produce a perfectly symmetric universe, but that tiny quantum fluctuations in the

inflaton are created. These tiny fluctuations form the primordial seeds for all structure created in the later universe. These fluctuations were first calculated byViatcheslav Mukhanov and G. V. Chibisov in theSoviet Union in analyzing Starobinsky's similar model. [*See Linde (1990) and Mukhanov (2005).*] [*cite journal|journal=JETP Lett.|volume=33|pages=532–5|year=1981|title=Quantum fluctuation and "nonsingular" universe|first=Viatcheslav F.|last=Mukhanov|coauthors=G. V. Chibisov*] [*cite journal|journal=Sov. Phys. JETP|volume=56|pages=258–65|year=1982|title=The vacuum energy and large scale structure of the universe|first=Viatcheslav F.|last=Mukhanov|coauthors=G. V. Chibisov*] In the context of inflation, they were worked out independently of the work of Mukhanov and Chibisov at the three-week 1982 Nuffield Workshop on the Very Early Universe at Cambridge University. [*See Guth (1997) for a description of the workshop.*] The fluctuations were calculated by four groups working separately over the course of the workshop:Stephen Hawking ; [*cite journal|title=The development of irregularities in a single bubble inflationary universe|first=S.W.|last=Hawking|journal=Phys.Lett.|volume=B115|pages=295|year=1982*] Starobinsky; [*cite journal|title=Dynamics of phase transition in the new inflationary universe scenario and generation of perturbations|first=Alexei A.|last=Starobinsky|journal=Phys. Lett.|volume=B117|pages=175–8|year=1982*] Guth andSo-Young Pi ; [*cite journal|title=Fluctuations in the new inflationary universe|first=A.H.|last=Guth|coauthor=S.Y. Pi|year=1982|journal=Phys. Rev. Lett.|volume=49|pages=1110–3|doi=10.1103/PhysRevLett.49.1110*] andJames M. Bardeen ,Paul Steinhardt and Michael Turner. [*cite journal|title=Spontaneous creation Of almost scale-free density perturbations in an inflationary universe|first=James M.|last=Bardeen|coauthors=Paul J. Steinhardt, Michael S. Turner|journal=Phys. Rev.|volume=D28|pages=679|year=1983*]**Observational status**Inflation is a concrete mechanism for realizing the

cosmological principle which is the basis of the standard model of physical cosmology: it accounts for the homogeneity and isotropy of the observable universe. In addition, it accounts for the observed flatness and absence of magnetic monopoles. Since Guth's early work, each of these observations has received further confirmation, most impressively by the detailed observations of thecosmic microwave background made by theWilkinson Microwave Anisotropy Probe (WMAP) satellite.See, "e.g." cite journal|last=Spergel|first=D.N.|coauthors="et al." (WMAP collaboration)|title=Three-year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Implications for cosmology|url=http://lambda.gsfc.nasa.gov/product/map/current/map_bibliography.cfm|year=2006] This analysis shows that the universe is flat to an accuracy of at least a few percent, and that it is homogeneous and isotropic to a part in 10,000.In addition, inflation predicts that the structures visible in the universe today formed through the

gravitational collapse of perturbations which were formed as quantum mechanical fluctuations in the inflationary epoch. The detailed form of the spectrum of perturbations called a nearly-scale-invariantGaussian random field (or Harrison-Zel'dovich spectrum) is very specific and has only two free parameters, the amplitude of the spectrum and the "spectral index" which measures the slight deviation from scale invariance predicted by inflation (perfect scale invariance corresponds to the idealized de Sitter universe). [*Perturbations can be represented by*] Inflation predicts that the observed perturbations should be inFourier modes of a givenwavelength . Each Fourier mode is normally distributed (usually called Gaussian) with mean zero. Different Fourier components are uncorrelated. The variance of a mode depends only on its wavelength in such a way that within any given volume each wavelength contributes an equal amount of power to the spectrum of perturbations. Since the Fourier transform is in three dimensions, this means that the variance of a mode goes as "k"^{−3}to compensate for the fact that within any volume, the number of modes with a given wavenumber "k" goes as "k"³.thermal equilibrium with each other (these are called "adiabatic" or "isentropic" perturbations). This structure for the perturbations has been confirmed by the WMAP satellite and other cosmic microwave background experiments, andgalaxy survey s, especially the ongoingSloan Digital Sky Survey .cite journal|first=M.|last=Tegmark|coauthors="et al." (SDSS collaboration)|title=Cosmological constraints from the SDSS luminous red galaxies|url=http://arxiv.org/abs/astro-ph/0608632|year=2006|month=August] These experiments have shown that the one part in 10,000 inhomogeneities observed have exactly the form predicted by theory. Moreover, the slight deviation from scale invariance has been measured. The "spectral index", "n"_{s}is equal to one for a scale-invariant spectrum. The simplest models of inflation predict that this quantity is between 0.92 and 0.98.cite journal|title=Cosmological perturbations: Myths and facts|journal=Mod. Phys. Lett.|volume=A19|pages=967–82|year=2004|first=Paul J.|last=Steinhardt|url=http://www.worldscinet.com/mpla/19/1913n16/S0217732304014252.html] cite journal|journal=Phys. Rev. Lett.|volume=96|year=2006|pages=111301|first=Latham A.|last=Boyle|coauthors=Paul J. Steinhardt and Neil Turok|title=Inflationary predictions for scalar and tensor fluctuations reconsidered|doi=10.1103/PhysRevLett.96.111301] cite journal|first=Max|last=Tegmark|title=What does inflation really predict? | doi = 10.1088/1475-7516/2005/04/001 |journal=JCAP|volume=0504|pages=001|year=2005|url=http://www.arxiv.org/abs/astro-ph/0410281] [*This is known as a "red" spectrum, in analogy to*] The WMAP satellite has measured "n"redshift , because the spectrum has more power at longer wavelengths._{s}= 0.960 ± 0.014 [*cite journal|title=WMAP gives thumbs-up to cosmological model|url=http://physicsworld.com/cws/article/news/33318|year=2008|month=March*] and shown that it is different from one at the level of twostandard deviation s (2σ). This is considered an important confirmation of the theory of inflation.A number of theories of inflation have been proposed that make radically different predictions, but they generally have much more fine tuning than is necessary. As a physical model, however, inflation is most valuable in that it robustly predicts the initial conditions of the universe based on only two adjustable parameters: the spectral index (that can only change in a small range) and the amplitude of the perturbations. Except in contrived models, this is true regardless of how inflation is realized in particle physics.

Occasionally, effects are observed that appear to contradict the simplest models of inflation. The first-year WMAP data suggested that the spectrum might not be nearly scale-invariant, but might instead have a slight curvature. [

*cite journal|first=D. N.|last=Spergel|coauthors="et al." (WMAP collaboration)|url=http://www.arxiv.org/astro-ph/0302209|title=First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: determination of cosmological parameters|journal=Astrophys. J. Suppl.|volume=148|pages=175|year=2003|doi=10.1086/377226*] However, the third-year data revealed that the effect was a statistical anomaly. Another effect has been remarked upon since the first cosmic microwave background satellite, theCosmic Background Explorer : the amplitude of thequadrupole moment of the cosmic microwave background is unexpectedly low and the other low multipoles appear to be preferentially aligned with theecliptic plane . Some have claimed that this is a signature of non-Gaussianity and thus contradicts the simplest models of inflation. Others have suggested that the effect may be due to other new physics, foreground contamination, or evenpublication bias . [*See*]cosmic microwave background#Low multipoles for details and references.An experimental program is underway to further test inflation with more precise measurements of the cosmic microwave background. In particular, high precision measurements of the so-called "B-modes" of the polarization of the background radiation will be evidence of the

gravitational radiation produced by inflation, and they will also show whether the energy scale of inflation predicted by the simplest models (10^{15}–10^{16}GeV ) is correct. These measurements are expected to be performed by the Planck satellite, although it is unclear if the signal will be visible, or if contamination from foreground sources will interfere with these measurements. [*cite conference|title=Systematic effects in CMB polarization measurements|first=C.|last=Rosset|coauthors=(PLANCK-HFI collaboration)|booktitle=Exploring the universe: Contents and structures of the universe (XXXIXth Rencontres de Moriond)|year=2005*] Other forthcoming measurements, such as those of21 centimeter radiation (radiation emitted and absorbed from neutral hydrogen before the first stars turned on), may measure the power spectrum with even greater resolution than the cosmic microwave background and galaxy surveys, although it is not known if these measurements will be possible or if interference with radio sources on earth and in the galaxy will be too great. [*cite journal|first=A.|last=Loeb|coauthors=and M. Zaldarriaga|title=Measuring the small-scale power spectrum of cosmic density fluctuations through 21 cm tomography prior to the epoch of structure formation|journal=Phys. Rev. Lett.|volume=92|pages=211301|year=2004|url=http://www.arxiv.org/abs/astro-ph/0312134|doi=10.1103/PhysRevLett.92.211301*]As of 2006, it is unclear what relationship if any the period of cosmic inflation has to do with

dark energy .Fact|date=February 2007 Dark energy is broadly similar to inflation, and is thought to be causing the expansion of the present-day universe to accelerate. However, the energy scale of dark energy is much lower, 10^{-12}GeV, roughly 27orders of magnitude less than the scale of inflation.**Theoretical status**In the early proposal of Guth, it was thought that the

inflaton was theHiggs field , the field which explains the mass of the elementary particles. It is now known that theinflaton cannot be the Higgs field.cite book

last = Guth

first = Alan

authorlink = Alan Guth

title = The Inflationary Universe

publisher =Addison-Wesley

year = 1997

isbn = 0201149427] Other models of inflation relied on the properties of grand unified theories. Since the simplest models ofgrand unification have failed, it is now thought by many physicists that inflation will be included in asupersymmetric theory likestring theory or a supersymmetric grand unified theory. A promising suggestion isbrane inflation . At present, however, whilst inflation is understood principally by its detailed predictions of the initial conditions for the hot early universe, the particle physics is largely "ad hoc" modelling. As such, despite the stringent observational tests inflation has passed, there are many open questions about the theory.**Fine-tuning problem**One of the most severe challenges for inflation arises from the need for

fine tuning in inflationary theories. In new inflation, the "slow-roll conditions" must be satisfied for inflation to occur. The slow-roll conditions say that theinflaton potential must be flat (compared to the largevacuum energy ) and that theinflaton particles must have a small mass. [*Technically, these conditions are that the*] In order for the new inflation theory of Linde, Albrecht and Steinhardt to be successful, therefore, it seemed that the universe must have a scalar field with an especially flat potential and special initial conditions.logarithmic derivative of the potential, $epsilon=(1/2)(V\text{'}/V)^2$ and second derivative $eta=V"/V-(1/2)(V\text{\'}/V)^2$ are small, where $V$ is the potential and the equations are written inreduced Planck units . See, "e.g." Liddle and Lyth (2000).**Andrei Linde**Andrei Linde proposed a theory known as "chaotic inflation" in which he suggested that the conditions for inflation are actually satisfied quite generically and inflation will occur in virtually any universe that begins in a chaotic, high energy state and has a scalar field with unbounded potential energy.cite journal|first=Andrei D.|last=Linde|title=Chaotic inflation | doi = 10.1088/1475-7516/2008/03/015 |journal=Phys. Lett.|volume=B129|pages=171–81|year=1983] However, in his model the

inflaton field necessarily takes values larger than one Planck unit: for this reason, these are often called "large field" models and the competing new inflation models are called "small field" models. In this situation, the predictions ofeffective field theory are thought to be invalid, andrenormalization should cause large corrections that could prevent inflation. [*Technically, this is because the*] This problem has not yet been resolved and some cosmologists argue that the small field models, in which inflation can occur at a much lower energy scale, are better models of inflation. [inflaton potential is expressed as a Taylor series in φ/"m"_{Pl}, where φ is theinflaton and "m"_{Pl}is the Planck mass. While for a single term, such as the mass term "m"_{φ}^{4}(φ/"m"_{Pl})², the slow roll conditions can be satisfied for φ much greater than "m"_{Pl}, this is precisely the situation in effective field theory in which higher order terms would be expected to contribute and destroy the conditions for inflation. The absence of these higher order corrections can be seen as another sort of fine tuning. See "e.g." cite journal|first=Laila|last=Alabidi|coauthors=and David H. Lyth|title=Inflation models and observation | doi = 10.1088/1475-7516/2006/05/016 |journal=JCAP|volume=0605|year=2006|pages=016|url=http://www.arxiv.org/abs/astro-ph/0510441*See, "e.g." cite journal|title=What would we learn by detecting a gravitational wave signal in the cosmic microwave background anisotropy? | doi = 10.1103/PhysRevLett.78.1861 |first=David H.|last=Lyth|journal=Phys. Rev. Lett.|volume=78|pages=1861–3|year=1997|id=arxiv|archive=hep-ph|id=9606387|url=http://www.slac.stanford.edu/spires/find/hep/www?rawcmd=FIND+EPRINT+HEP-PH/9606387*] While inflation depends on quantum field theory (and the semiclassical approximation toquantum gravity ) in an important way, it has not been completely reconciled with these theories.Robert Brandenberger has commented on fine-tuning in another situation. [*cite conference|title=Challenges for inflationary cosmology|first=Robert H.|last=Brandenberger|month=November | year=2004|booktitle=10th International Symposium on Particles, Strings and Cosmology|url=http://www.arxiv.org/abs/astro-ph/0411671*] The amplitude of the primordial inhomogeneities produced in inflation is directly tied to the energy scale of inflation. There are strong suggestions that this scale is around 10^{16}GeV or 10^{−3}times thePlanck energy . The natural scale is naïvely the Planck scale so this small value could be seen as another form of fine-tuning (called ahierarchy problem ): the energy density given by the scalar potential is down by 10^{−12}compared to thePlanck density . This is not usually considered to be a critical problem, however, because the scale of inflation corresponds naturally to the scale ofgauge unification .**Eternal inflation**Cosmic inflation seems to be eternal the way it is theorised. Although new inflation is classically rolling down the potential, quantum fluctuations can sometimes bring it back up to previous levels. These regions in which the

inflaton fluctuates upwards expand much faster than regions in which theinflaton has a lower potential energy, and tend to dominate in terms of physical volume. This steady state, which first developed by Vilenkin,cite journal|first=Alexander|last=Vilenkin|title=The birth of inflationary universes | doi = 10.1103/PhysRevD.27.2848 |journal=Phys. Rev.|volume=D27|pages=2848|year=1983] is called "eternal inflation". It has been shown that any inflationary theory with an unbounded potential is eternal. [*cite journal | author = A. Linde |title = Eternal chaotic inflation | journal = Mod. Phys. Lett. |volume = A1 |year =1986 | pages=81 cite journal | author = A. Linde |title = Eternally existing self-reproducing chaotic inflationary universe | journal = Phys. Lett. |volume = B175 |year =1986|pages=395–400*] It is a popular belief among physicists that this steady state cannot continue forever into the past. [*cite journal |author = A. Borde, A. Guth and A. Vilenkin |title = Inflationary space-times are incomplete in past directions|journal = Phys. Rev. Lett.|volume=90|year=2003|pages=151301 |doi = 10.1103/PhysRevLett.90.151301*] [*cite journal |author = A. Borde |title = Open and closed universes, initial singularities and inflation|journal = Phys. Rev. |volume=D50|year=1994|pages=3692–702*] [*cite journal |author = A. Borde and A. Vilenkin |title = Eternal inflation and the initial singularity|journal = Phys. Rev. Lett.|volume=72|year=1994|pages=3305–9 |doi = 10.1103/PhysRevLett.72.3305*] The inflationary spacetime, which is similar tode Sitter space , is incomplete without a contracting region. However, unlike de Sitter space, fluctuations in a contracting inflationary space will collapse to form agravitational singularity , a point where densities become infinite. Therefore, it is necessary to have a theory for the universe's initial conditions. Linde, however, believes inflation may be past eternal. [*Linde (2005, §V).*]**Initial conditions**Some physicists have tried to avoid the initial conditions problem by proposing models for an eternally inflating universe with no origin. [

*cite journal|title=Does inflation provide natural initial conditions for the universe?|first=Sean M.|last=Carroll|journal=Gen. Rel. Grav.|volume=37|pages=1671–4|year=2005|url=http://www.arxiv.org/abs/gr-qc/0505037|doi=10.1007/s10714-005-0148-2*] [*cite journal|title=Spontaneous inflation and the origin of the arrow of time|first=Sean M.|last=Carroll|url=http://www.arxiv.org/abs/hep-th/0410270*] [*Anthony Aguirre, Steven Gratton, "Inflation without a beginning: A null boundary proposal", Phys.Rev. D67 (2003) 083515, [*] [*http://arxiv.org/abs/gr-qc/0301042*]*Anthony Aguirre, Steven Gratton, "Steady-State Eternal Inflation", Phys.Rev. D65 (2002) 083507, [*] These models propose that whilst the universe, on the largest scales, expands exponentially it is always spatially infinite and has existed, and will exist, forever.*http://arxiv.org/abs/astro-ph/0111191*]Other proposals attempt to describe the ex nihilo creation of the universe

quantum cosmology and the following inflation. Vilenkin put forth one such scenario. Hartle and Hawking offered theno-boundary proposal for the initial creation of the universe in which inflation comes about naturally. [*J. Hartle and S. W. Hawking, "Wave function of the universe", "Phys. Rev."*]**D28**, 2960 (1983). See also Hawking (1998).Alan Guth has described the inflationary universe as the "ultimate free lunch": [*Hawking (1998), p. 129. [*] new universes, similar to our own, are continually produced in a vast inflating background. Gravitational interactions, in this case, circumvent (but do not violate) neither the*http://en.wikiquote.org/wiki/Alan_Guth Wikiquote*]first law of thermodynamics (energy conservation ) nor thesecond law of thermodynamics (entropy and thearrow of time problem). However, while there is consensus that this solves the initial conditions problem, some have disputed this, as it is much more likely that the universe came about by a quantum fluctuation. Donald Page was an outspoken critic of inflation because of this anomaly. [*D.N. Page, "Inflation does not explain time asymmetry", "Nature",*] He stressed that the thermodynamic**304**, 39 (1983) see alsoRoger Penrose 's book .arrow of time necessitates lowentropy initial conditions, which would be highly unlikely. According to them, rather than solving this problem, the inflation theory further aggravates it – the reheating at the end of the inflation era increases entropy, making it necessary for the initial state of the Universe to be even more orderly than in other Big Bang theories with no inflation phase.Hawking and Page later found ambiguous results when they attempted to compute the probability of inflation in the Hartle-Hawking initial state. [

*cite journal|title=How probable is inflation?|first=S. W.|last=Hawking|coauthors=Don. N. Page|year=1988|volume=B298|pages=789|journal=Nucl. Phys.|doi=10.1016/0550-3213(88)90008-9*] Other authors have argued that, since inflation is eternal, the probability doesn't matter as long as it is not precisely zero: once it starts, inflation perpetuates itself and quickly dominates the universe.Fact|date=February 2007 However, Albrecht and Lorenzo Sorbo have argued that the probability of an inflationary cosmos, consistent with today's observations, emerging by a random fluctuation from some pre-existent state, "compared" with a non-inflationary cosmos overwhelmingly favours the inflationary scenario, simply because the "seed" amount of non-gravitational energy required for the inflationary cosmos is so much less than any required for a non-inflationary alternative, which outweighs any entropic considerations. [*cite journal|first=Andreas|last=Albrecht|coauthors=Lorenzo Sorbo|title=Can the universe afford inflation?|journal=Physical Review|volume=D70|pages=063528|year=2004|url=http://www.arxiv.org/abs/hep-th/0405270*]Another problem that has occasionally been mentioned is the trans-Planckian problem or trans-Planckian effects. [

*cite journal|first=Jerome|last=Martin|coauthors=and Robert H. Brandenberger|title=The trans-Planckian problem of inflationary cosmology|journal=Phys. Rev.|volume=D63|year=2001|pages=123501|url=http://www.arxiv.org/abs/hep-th/0005209|doi=10.1103/PhysRevD.63.123501*] Since the energy scale of inflation and the Planck scale are relatively close, some of the quantum fluctuations which have made up the structure in our universe were smaller than the Planck length before inflation. Therefore, there ought to be corrections from Planck-scale physics, in particular the unknown quantum theory of gravity. There has been some disagreement about the magnitude of this effect: about whether it is just on the threshold of detectability or completely undetectable. [*cite journal|first=Jerome|last=Martin|coauthors=and Christophe Ringeval|title=Superimposed Oscillations in the WMAP Data?|journal=Phys. Rev.|volume=D69|year=2004|pages=083515|url=http://www.arxiv.org/abs/astro-ph/0310382|doi=10.1103/PhysRevD.69.083515*]**Reheating**The end of inflation is called reheating or thermalization because the large potential energy decays into particles and fills the universe with radiation. Because the nature of the

inflaton is not known, this process is still poorly understood, although it is believed to take place through aparametric resonance . [*See Kolb and Turner (1988) or Mukhanov (2005).*] [*cite journal|title=Reheating after inflation | doi = 10.1088/0264-9381/3/5/011 |first=Lev|last=Kofman|journal=Phys. Rev. Lett.|volume=73|year=1994|pages=3195–3198|url=http://www.arxiv.org/abs/hep-th/9405187|unused_data=|coauthors Andri Linde and Alexei Starobinsky*]**Non-eternal inflation**Another kind of inflation, called "hybrid inflation", is an extension of new inflation. It introduces additional scalar fields, so that while one of the scalar fields is responsible for normal slow roll inflation, another triggers the end of inflation: when inflation has continued for sufficiently long, it becomes favorable to the second field to decay into a much lower energy state. [

*Robert H. Brandenberger, "A Status Review of Inflationary Cosmology", proceedingsJournal-ref: BROWN-HET-1256 (2001), (available from arxiv|archive=hep-ph|id=0101119 v1 11 Jan 2001)*] Unlike most other models of inflation, many versions of hybrid inflation are not eternal. [*Andrei Linde, "Prospects of Inflation", "Physica Scripta Online" (2004) (available from arxiv|archive=hep-th|id=0402051 )*] [*Blanco-Pillado et al. , "Racetrack inflation", (2004) (available from arxiv|archive=hep-th|id=0406230 )*]In hybrid inflation, one of the scalar fields is responsible for most of the energy density (thus determining the rate of expansion), while the other is responsible for the slow roll (thus determining the period of inflation and its termination). Thus fluctuations in the former inflaton would not affect inflation termination, while fluctuations in the latter would not affect the rate of expansion. Therefore hybrid inflation is not eternal. When the second (slow-rolling) inflaton reaches the bottom of its potential, it changes the location of the minimum of the first inflaton's potential, which leads to a fast roll of the inflaton down its potential, leading to termination of inflation.

**Inflation and string cosmology**The discovery of

flux compactification s have opened the way for reconciling inflation and string theory. [*cite journal|title=Towards inflation in string theory|first=Shamit|last=Kachru|coauthors=Renata Kallosh, Andrei Linde, Juan M. Maldacena, Liam McAllister and Sandip P. Trivedi|year=2003|journal=JCAP|volume=0310|pages=013|url=http://www.arxiv.org/abs/hep-th/0308055*] A new theory, calledbrane inflation suggests that inflation arises from the motion ofD-brane s [*G. R. Dvali, S. H. Henry Tye, "Brane inflation," "Phys.Lett."*] in the compactified geometry, usually towards a stack of anti-D-branes. This theory, governed by the**B450**, 72-82 (1999), arxiv|archive=hep-ph|id=9812483.Dirac-Born-Infeld action , is very different from ordinary inflation. The dynamics are not completely understood. It appears that special conditions are necessary since inflation occurs in tunneling between two vacua in thestring landscape . The process of tunneling between two vacua is a form of old inflation, but new inflation must then occur by some other mechanism.**Alternatives to inflation**String theory requires that, in addition to the three spatial dimensions we observe, there exist additional dimensions that are curled up or compactified (see alsoKaluza-Klein theory ). Extra dimensions appear as a frequent component ofsupergravity models and other approaches toquantum gravity . This raises the question of why four space-time dimensions became large and the rest became unobservably small. An attempt to address this question, calledstring gas cosmology , was proposed byRobert Brandenberger andCumrun Vafa . [*Robert H. Brandenberger and C. Vafa, "Superstrings in the early universe," "Nucl. Phys."*] This model focuses on the dynamics of the early universe considered as a hot gas of strings. Brandenberger and Vafa show that a dimension of**B316**, 391 (1989)spacetime can only expand if the strings that wind around it can efficiently annihilate each other. Each string is a one-dimensional object, and the largest number of dimensions in which two strings will generically intersect (and, presumably, annihilate) is three. Therefore, one argues that the most likely number of non-compact (large) spatial dimensions is three. Current work on this model centers on whether it can succeed in stabilizing the size of the compactified dimensions and produce the correct spectrum of primordial density perturbations. For a recent review, see [*Thorsten Battefeld and Scott Watson, "String Gas Cosmology", "Rev. Mod. Phys"*] [**78**, 435-454 (2006)*Robert H. Brandenberger, Ali Nayeri, Subodh P. Patil and Cumrun Vafa, "String Gas Cosmology and Structure Formation", Int.J.Mod.Phys.A22:3621-3642,2007. , arxiv|archive=hep-th|id=0608121.*]The

ekpyrotic andcyclic model s are also considered competitors to inflation. These models solve thehorizon problem through an expanding epoch well "before" the Big Bang, and then generate the required spectrum of primordial density perturbations during a contracting phase leading to aBig Crunch . The universe passes through the Big Crunch and emerges in a hotBig Bang phase. In this sense they are reminiscent of theoscillatory universe proposed byRichard Chace Tolman : however in Tolman's model the total age of the universe is necessarily finite, while in these models this is not necessarily so. Whether the correct spectrum of density fluctuations can be produced, and whether the universe can successfully navigate the Big Bang/Big Crunch transition, remains a topic of controversy and current research.**ee also***

Brane cosmology

*Varying speed of light

*Dark flow **Notes****References***cite book |first=Alan|last=Guth|authorlink=Alan Guth|title=The Inflationary Universe: The Quest for a New Theory of Cosmic Origins|isbn=0-201-32840-2|publisher=Perseus|year=1997

*cite book|first=Stephen|last=Hawking|authorlink=Stephen Hawking|title=A Brief History of Time|isbn=0-553-38016-8|publisher=Bantam|year=1998

*cite book | first = Edward | last = Kolb | coauthors = Michael Turner | title = The Early Universe | publisher = Addison-Wesley | year = 1988 | isbn = 0-201-11604-9

*cite book|last=Linde|first=Andrei|authorlink=Andrei Linde|url=http://arxiv.org/abs/hep-th/0503203|title=Particle Physics and Inflationary Cosmology|publisher=Harwood|location=Chur, Switzerland|year=1990

*Linde, Andrei (2005) "Inflation and String Cosmology," "eConf"**C040802**(2004) L024; "J. Phys. Conf. Ser."**24**(2005) 151–60; arxiv|archive=hep-th|id=0503195 v12005-03-24 .

*cite book | first = Andrew | last = Liddle | coauthors = David Lyth | title = Cosmological Inflation and Large-Scale Structure | publisher = Cambridge | year = 2000 | isbn = 0-521-57598-2

*cite journal|first=David H.|last=Lyth|coauthor=Antonio Riotto|title=Particle physics models of inflation and the cosmological density perturbation | doi = 10.1016/S0370-1573(98)00128-8 |year=1999|journal=Phys. Rept.|url=http://www.slac.stanford.edu/spires/find/hep/www?rawcmd=FIND+EPRINT+HEP-PH/9807278|volume=314|pages=1–146

*cite book | first = Viatcheslav | last = Mukhanov | title = Physical Foundations of Cosmology | publisher = Cambridge University Press | year = 2005 | isbn = 0-521-56398-4

*cite book | first = Alex | last = Vilenkin | authorlink=Alex Vilenkin | title= Many Worlds in One: The Search for Other Universes | publisher = Hill and Wang | year = 2006 | isbn = 0809095238

*cite book | first = P. J. E. | last = Peebles |authorlink=Philip James Edwin Peebles| title = Principles of Physical Cosmology | publisher = Princeton University Press | year = 1993 | isbn = 0-691-01933-9**External links*** [

*http://nedwww.ipac.caltech.edu/level5/Guth/Guth_contents.html Was Cosmic Inflation The 'Bang' Of The Big Bang?*] , by Alan Guth, 1997

* [*http://arxiv.org/abs/astro-ph/9901124 An Introduction to Cosmological Inflation*] by Andrew Liddle, 1999

* [*http://www2.iap.fr/Conferences/Colloque/col2004/Docs/20040628_liddle.pdf update 2004*] by Andrew Liddle

* [*http://arxiv.org/abs/hep-ph/0309238 hep-ph/0309238 Laura Covi: Status of observational cosmology and inflation*]

* [*http://arxiv.org/abs/hep-th/0311040 hep-th/0311040 David H. Lyth: Which is the best inflation model?*]

* [*http://www.symmetrymag.org/cms/?pid=1000045 The Growth of Inflation*] "Symmetry", December 2004

* [*http://www.symmetrymag.org/cms/?pid=1000037 Guth's logbook showing the original idea*]

* [*http://skyandtelescope.com/news/article_1697_1.asp WMAP Bolsters Case for Cosmic Inflation, March 2006*]

* [*http://www.nasa.gov/home/hqnews/2006/mar/HQ_06097_first_trillionth_WMAP.html NASA March 2006 WMAP press release*]

*Wikimedia Foundation.
2010.*

### Look at other dictionaries:

**cosmic inflation**— /kɒzmɪk inˈfleɪʃən/ (say kozmik in flayshuhn) noun the extreme accelerated expansion of the universe theorised to have occurred in its very early stages after the big bang, responsible for the universe being flat, isotropic and homogenous … Australian English dictionary**Inflation (cosmology)**— Inflation model and Inflation theory redirect here. For a general rise in the price level, see Inflation. For other uses, see Inflation (disambiguation). Physical cosmology … Wikipedia**Cosmic microwave background experiments**— [ Cosmic background (CMB) temperature on the celestial sphere as determined with the COBE satellite, (top) uncorrected, (middle) corrected for the dipole term due to our peculiar velocity, (bottom) corrected for contributions from the dipole term … Wikipedia**Cosmic microwave background radiation**— CMB and Cosmic background radiation redirect here. For other uses see CMB (disambiguation) and Cosmic background (disambiguation). Physical cosmology … Wikipedia**Cosmic variance**— For the weblog, see Cosmic Variance (blog). Physical cosmology Universe … Wikipedia**Cosmic gravitational wave background**— Physical cosmology Universe · Big Bang … Wikipedia**Cosmic string**— Not to be confused with string in string theory. Cosmic strings are hypothetical 1 dimensional (spatially) topological defects which may have formed during a symmetry breaking phase transition in the early universe when the topology of the vacuum … Wikipedia**Cosmic neutrino background**— Physical cosmology Universe · Big Bang … Wikipedia**Chaotic Inflation theory**— Physical cosmology Universe · Big Bang … Wikipedia**Non-minimally coupled inflation**— is an inflationary model in which the constant which couples gravity to the inflaton field is not small. The coupling constant is usually represented by ξ, which features in the action (constructed by modifying the Einstein Hilbert action):[1] ξ… … Wikipedia