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class="interlanguage-link-target"><span>فارسی</span></a></li><li class="interlanguage-link interwiki-fr badge-Q70893996 mw-list-item" title=""><a href="https://fr.wikipedia.org/wiki/Inflation_%C3%A9ternelle" title="Inflation éternelle – French" lang="fr" hreflang="fr" data-title="Inflation éternelle" data-language-autonym="Français" data-language-local-name="French" class="interlanguage-link-target"><span>Français</span></a></li><li class="interlanguage-link interwiki-ko mw-list-item"><a href="https://ko.wikipedia.org/wiki/%EC%98%81%EC%9B%90%ED%95%9C_%EA%B8%89%ED%8C%BD%EC%B0%BD_%EC%9D%B4%EB%A1%A0" title="영원한 급팽창 이론 – Korean" lang="ko" hreflang="ko" data-title="영원한 급팽창 이론" data-language-autonym="한국어" data-language-local-name="Korean" class="interlanguage-link-target"><span>한국어</span></a></li><li class="interlanguage-link interwiki-it mw-list-item"><a href="https://it.wikipedia.org/wiki/Inflazione_eterna" title="Inflazione eterna – Italian" lang="it" hreflang="it" data-title="Inflazione 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<div class="mw-indicators"> </div> <div id="siteSub" class="noprint">From Wikipedia, the free encyclopedia</div> </div> <div id="contentSub"><div id="mw-content-subtitle"></div></div> <div id="mw-content-text" class="mw-body-content"><div class="mw-content-ltr mw-parser-output" lang="en" dir="ltr"><div class="shortdescription nomobile noexcerpt noprint searchaux" style="display:none">Hypothetical inflationary universe model</div> <p class="mw-empty-elt"> </p><p><b>Eternal inflation</b> is a hypothetical <a href="/wiki/Inflation_(cosmology)" class="mw-redirect" title="Inflation (cosmology)">inflationary universe</a> model, which is itself an outgrowth or extension of the <a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a> theory. </p><p>According to eternal inflation, the inflationary phase of the universe's expansion lasts forever throughout most of the universe. Because the regions expand exponentially rapidly, most of the volume of the universe at any given time is inflating. Eternal inflation, therefore, produces a hypothetically infinite <a href="/wiki/Multiverse" title="Multiverse">multiverse</a>, in which only an insignificant <a href="/wiki/Fractal" title="Fractal">fractal</a> volume ends inflation. </p><p><a href="/wiki/Paul_Steinhardt" title="Paul Steinhardt">Paul Steinhardt</a>, one of the original researchers of the inflationary model, introduced the first example of eternal inflation in 1983,<sup id="cite_ref-steinhardt_1-0" class="reference"><a href="#cite_note-steinhardt-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> and <a href="/wiki/Alexander_Vilenkin" title="Alexander Vilenkin">Alexander Vilenkin</a> showed that it is generic.<sup id="cite_ref-vilenkin_2-0" class="reference"><a href="#cite_note-vilenkin-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup><sup class="noprint Inline-Template" style="margin-left:0.1em; white-space:nowrap;">[<i><a href="/wiki/Wikipedia:Please_clarify" title="Wikipedia:Please clarify"><span title="The text near this tag may need clarification or removal of jargon. (September 2023)">clarification needed</span></a></i>]</sup> </p><p><a href="/wiki/Alan_Guth" title="Alan Guth">Alan Guth</a>'s 2007 paper, "Eternal inflation and its implications",<sup id="cite_ref-eternal_3-0" class="reference"><a href="#cite_note-eternal-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> states that under reasonable assumptions "Although inflation is generically eternal into the future, it is not eternal into the past." Guth detailed what was known about the subject at the time, and demonstrated that eternal inflation was still considered the likely outcome of inflation, more than 20 years after eternal inflation was first introduced by Steinhardt. </p> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Overview">Overview</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Eternal_inflation&action=edit&section=1" title="Edit section: Overview"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <div class="mw-heading mw-heading3"><h3 id="Development_of_the_theory">Development of the theory</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Eternal_inflation&action=edit&section=2" title="Edit section: Development of the theory"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r1236090951">.mw-parser-output .hatnote{font-style:italic}.mw-parser-output div.hatnote{padding-left:1.6em;margin-bottom:0.5em}.mw-parser-output .hatnote i{font-style:normal}.mw-parser-output .hatnote+link+.hatnote{margin-top:-0.5em}@media print{body.ns-0 .mw-parser-output .hatnote{display:none!important}}</style><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Bubble_nucleation" class="mw-redirect" title="Bubble nucleation">Bubble nucleation</a></div> <p>Inflation, or the inflationary universe theory, was originally developed as a way to overcome the few remaining problems with what was otherwise considered a successful theory of cosmology, the Big Bang model. </p><p>In 1979, Alan Guth introduced the inflationary model of the universe to explain why the universe is flat and homogeneous (which refers to the smooth distribution of matter and radiation on a large scale).<sup id="cite_ref-4" class="reference"><a href="#cite_note-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> The basic idea was that the universe underwent a period of rapidly accelerating expansion a few instants after the Big Bang. He offered a mechanism for causing the inflation to begin: <a href="/wiki/False_vacuum" title="False vacuum">false vacuum</a> energy. Guth coined the term "inflation," and was the first to discuss the theory with other scientists worldwide. </p><p>Guth's original formulation was problematic, as there was no consistent way to bring an end to the inflationary epoch and end up with the hot, <a href="/wiki/Isotropic" class="mw-redirect" title="Isotropic">isotropic</a>, homogeneous universe observed today. Although the false vacuum could decay into empty "bubbles" of "true vacuum" that expanded at the speed of light, the empty bubbles could not coalesce to reheat the universe, because they could not keep up with the remaining inflating universe. </p><p>In 1982, this "<a href="/wiki/Graceful_exit_problem_(cosmology)" class="mw-redirect" title="Graceful exit problem (cosmology)">graceful exit problem</a>" was solved independently by <a href="/wiki/Andrei_Linde" title="Andrei Linde">Andrei Linde</a> and by <a href="/wiki/Andreas_Albrecht_(cosmologist)" title="Andreas Albrecht (cosmologist)">Andreas Albrecht</a> and Paul J. Steinhardt<sup id="cite_ref-journals.aps.org_5-0" class="reference"><a href="#cite_note-journals.aps.org-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> who showed how to end inflation without making empty bubbles and, instead, end up with a hot expanding universe. The basic idea was to have a continuous "slow-roll" or slow evolution from false vacuum to true without making any bubbles. The improved model was called "new inflation." </p><p>In 1983, Paul Steinhardt was the first to show that this "new inflation" does not have to end everywhere.<sup id="cite_ref-steinhardt_1-1" class="reference"><a href="#cite_note-steinhardt-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> Instead, it might only end in a finite patch or a hot bubble full of matter and radiation, and that inflation continues in most of the universe while producing hot bubble after hot bubble along the way. Alexander Vilenkin showed that when quantum effects are properly included, this is actually generic to all new inflation models.<sup id="cite_ref-vilenkin_2-1" class="reference"><a href="#cite_note-vilenkin-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> </p><p>Using ideas introduced by Steinhardt and Vilenkin, Andrei Linde published an alternative model of inflation in 1986 which used these ideas to provide a detailed description of what has become known as the Chaotic Inflation theory or eternal inflation.<sup id="cite_ref-6" class="reference"><a href="#cite_note-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Quantum_fluctuations">Quantum fluctuations</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Eternal_inflation&action=edit&section=3" title="Edit section: Quantum fluctuations"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>New inflation does not produce a perfectly symmetric universe due to quantum fluctuations during inflation. The fluctuations cause the energy and matter density to be different at different points in space. </p><p>Quantum fluctuations in the hypothetical inflaton field produce changes in the rate of expansion that are responsible for eternal inflation. Those regions with a higher rate of inflation expand faster and dominate the universe, despite the natural tendency of inflation to end in other regions. This allows inflation to continue forever, to produce future-eternal inflation. As a simplified example, suppose that during inflation, the natural decay rate of the <a href="/wiki/Inflaton" title="Inflaton">inflaton</a> field is slow compared to the effect of quantum fluctuation. When a mini-universe inflates and "self-reproduces" into, say, twenty causally-disconnected mini-universes of equal size to the original mini-universe, perhaps nine of the new mini-universes will have a larger, rather than smaller, average inflaton field value than the original mini-universe, because they inflated from regions of the original mini-universe where quantum fluctuation pushed the inflaton value up more than the slow inflation decay rate brought the inflaton value down. Originally there was one mini-universe with a given inflaton value; now there are nine mini-universes that have a slightly larger inflaton value. (Of course, there are also eleven mini-universes where the inflaton value is slightly lower than it originally was.) Each mini-universe with the larger inflaton field value restarts a similar round of approximate self-reproduction within itself. (The mini-universes with lower inflaton values may also reproduce, unless its inflaton value is small enough that the region drops out of inflation and ceases self-reproduction.) This process continues indefinitely; nine high-inflaton mini-universes might become 81, then 729... Thus, there is eternal inflation.<sup id="cite_ref-7" class="reference"><a href="#cite_note-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> </p><p>In 1980, quantum fluctuations were suggested by <a href="/wiki/Viatcheslav_Mukhanov" title="Viatcheslav Mukhanov">Viatcheslav Mukhanov</a> and <a href="/wiki/Gennady_Chibisov" title="Gennady Chibisov">Gennady Chibisov</a><sup id="cite_ref-8" class="reference"><a href="#cite_note-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-9" class="reference"><a href="#cite_note-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> in the context of a model of modified gravity by <a href="/wiki/Alexei_Starobinsky" title="Alexei Starobinsky">Alexei Starobinsky</a><sup id="cite_ref-10" class="reference"><a href="#cite_note-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup> to be possible seeds for forming galaxies. </p><p>In the context of inflation, quantum fluctuations were first analyzed at the three-week 1982 Nuffield Workshop on the Very Early Universe at Cambridge University.<sup id="cite_ref-11" class="reference"><a href="#cite_note-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> The average strength of the fluctuations was first calculated by four groups working separately over the course of the workshop: <a href="/wiki/Stephen_Hawking" title="Stephen Hawking">Stephen Hawking</a>;<sup id="cite_ref-12" class="reference"><a href="#cite_note-12"><span class="cite-bracket">[</span>12<span class="cite-bracket">]</span></a></sup> Starobinsky;<sup id="cite_ref-13" class="reference"><a href="#cite_note-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup> Guth and <a href="/wiki/So-Young_Pi" title="So-Young Pi">So-Young Pi</a>;<sup id="cite_ref-14" class="reference"><a href="#cite_note-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup> and <a href="/wiki/James_M._Bardeen" title="James M. Bardeen">James M. Bardeen</a>, <a href="/wiki/Paul_Steinhardt" title="Paul Steinhardt">Paul Steinhardt</a> and <a href="/wiki/Michael_Turner_(cosmologist)" class="mw-redirect" title="Michael Turner (cosmologist)">Michael Turner</a>.<sup id="cite_ref-15" class="reference"><a href="#cite_note-15"><span class="cite-bracket">[</span>15<span class="cite-bracket">]</span></a></sup> </p><p>The early calculations derived at the Nuffield Workshop only focused on the average fluctuations, whose magnitude is too small to affect inflation. However, beginning with the examples presented by Steinhardt<sup id="cite_ref-steinhardt_1-2" class="reference"><a href="#cite_note-steinhardt-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> and Vilenkin,<sup id="cite_ref-vilenkin_2-2" class="reference"><a href="#cite_note-vilenkin-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> the same quantum physics was later shown to produce occasional large fluctuations that increase the rate of inflation and keep inflation going eternally. </p> <div class="mw-heading mw-heading3"><h3 id="Further_developments">Further developments</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Eternal_inflation&action=edit&section=4" title="Edit section: Further developments"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>In analyzing the Planck Satellite data from 2013, Anna Ijjas and Paul Steinhardt showed that the simplest textbook inflationary models were eliminated and that the remaining models require exponentially more tuned starting conditions, more parameters to be adjusted, and less inflation. Later Planck observations reported in 2015 confirmed these conclusions.<sup id="cite_ref-16" class="reference"><a href="#cite_note-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-17" class="reference"><a href="#cite_note-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup> </p><p>A 2014 paper by Kohli and Haslam called into question the viability of the eternal inflation theory, by analyzing Linde's chaotic inflation theory in which the quantum fluctuations are modeled as Gaussian white noise.<sup id="cite_ref-18" class="reference"><a href="#cite_note-18"><span class="cite-bracket">[</span>18<span class="cite-bracket">]</span></a></sup> They showed that in this popular scenario, eternal inflation in fact cannot be eternal, and the random noise leads to spacetime being filled with singularities. This was demonstrated by showing that solutions to the Einstein field equations diverge in a finite time. Their paper therefore concluded that the theory of eternal inflation based on random quantum fluctuations would not be a viable theory, and the resulting existence of a multiverse is "still very much an open question that will require much deeper investigation". </p> <div class="mw-heading mw-heading2"><h2 id="Inflation,_eternal_inflation,_and_the_multiverse"><span id="Inflation.2C_eternal_inflation.2C_and_the_multiverse"></span>Inflation, eternal inflation, and the multiverse</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Eternal_inflation&action=edit&section=5" title="Edit section: Inflation, eternal inflation, and the multiverse"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>In 1983, it was shown that inflation could be eternal, leading to a <a href="/wiki/Multiverse" title="Multiverse">multiverse</a> in which space is broken up into bubbles or patches whose properties differ from patch to patch spanning all physical possibilities. </p><p>Paul Steinhardt, who produced the first example of eternal inflation,<sup id="cite_ref-steinhardt_1-3" class="reference"><a href="#cite_note-steinhardt-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> eventually became a strong and vocal opponent of the theory. He argued that the multiverse represented a breakdown of the inflationary theory, because, in a multiverse, any outcome is equally possible, so inflation makes no predictions and, hence, is untestable. Consequently, he argued, inflation fails a key condition for a <a href="/wiki/Scientific_theory" title="Scientific theory">scientific theory</a>.<sup id="cite_ref-Inflation_Debate_19-0" class="reference"><a href="#cite_note-Inflation_Debate-19"><span class="cite-bracket">[</span>19<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-20" class="reference"><a href="#cite_note-20"><span class="cite-bracket">[</span>20<span class="cite-bracket">]</span></a></sup> </p><p>Both Linde and Guth, however, continued to support the inflationary theory and the multiverse. Guth declared: </p> <style data-mw-deduplicate="TemplateStyles:r1244412712">.mw-parser-output .templatequote{overflow:hidden;margin:1em 0;padding:0 32px}.mw-parser-output .templatequotecite{line-height:1.5em;text-align:left;margin-top:0}@media(min-width:500px){.mw-parser-output .templatequotecite{padding-left:1.6em}}</style><blockquote class="templatequote"><p>It's hard to build models of inflation that don't lead to a multiverse. It's not impossible, so I think there's still certainly research that needs to be done. But most models of inflation do lead to a multiverse, and evidence for inflation will be pushing us in the direction of taking the idea of a multiverse seriously.<sup id="cite_ref-Kramer_21-0" class="reference"><a href="#cite_note-Kramer-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup></p></blockquote> <p>According to Linde, "It's possible to invent models of inflation that do not allow a multiverse, but it's difficult. Every experiment that brings better credence to inflationary theory brings us much closer to hints that the multiverse is real."<sup id="cite_ref-Kramer_21-1" class="reference"><a href="#cite_note-Kramer-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup> </p><p>In 2018 the late <a href="/wiki/Stephen_Hawking" title="Stephen Hawking">Stephen Hawking</a> and <a href="/wiki/Thomas_Hertog" title="Thomas Hertog">Thomas Hertog</a> published a paper in which the need for an infinite multiverse vanishes as Hawking says their theory gives universes which are "reasonably smooth and globally finite".<sup id="cite_ref-22" class="reference"><a href="#cite_note-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-23" class="reference"><a href="#cite_note-23"><span class="cite-bracket">[</span>23<span class="cite-bracket">]</span></a></sup> The theory uses the <a href="/wiki/Holographic_principle" title="Holographic principle">holographic principle</a> to define an 'exit plane' from the timeless state of eternal inflation. The universes which are generated on the plane are described using a redefinition of the <a href="/wiki/Hartle%E2%80%93Hawking_state" title="Hartle–Hawking state">no-boundary</a> wavefunction - in fact the theory requires a boundary at the beginning of time.<sup id="cite_ref-24" class="reference"><a href="#cite_note-24"><span class="cite-bracket">[</span>24<span class="cite-bracket">]</span></a></sup> Stated simply Hawking says that their findings "imply a significant reduction of the multiverse" which as the University of Cambridge points out, makes the theory "predictive and testable" using <a href="/wiki/Gravitational-wave_astronomy" title="Gravitational-wave astronomy">gravitational wave astronomy</a>.<sup id="cite_ref-25" class="reference"><a href="#cite_note-25"><span class="cite-bracket">[</span>25<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="See_also">See also</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Eternal_inflation&action=edit&section=6" title="Edit section: See also"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a href="/wiki/Astrophysics" title="Astrophysics">Astrophysics</a></li> <li><a href="/wiki/Cosmology" title="Cosmology">Cosmology</a></li> <li><a href="/wiki/Inflation_(cosmology)" class="mw-redirect" title="Inflation (cosmology)">Inflation (cosmology)</a></li> <li><a href="/wiki/Fractal_cosmology" title="Fractal cosmology">Fractal cosmology</a></li> <li><a href="/wiki/Physical_cosmology" title="Physical cosmology">Physical cosmology</a></li> <li><a href="/wiki/Shape_of_the_universe" title="Shape of the universe">Shape of the universe</a></li> <li><a href="/wiki/False_vacuum" title="False vacuum">False vacuum</a></li> <li><a href="/wiki/Measure_problem_(cosmology)" title="Measure problem (cosmology)">Measure problem (cosmology)</a></li></ul> <div class="mw-heading mw-heading2"><h2 id="References">References</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Eternal_inflation&action=edit&section=7" title="Edit section: References"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r1239543626">.mw-parser-output .reflist{margin-bottom:0.5em;list-style-type:decimal}@media screen{.mw-parser-output .reflist{font-size:90%}}.mw-parser-output .reflist .references{font-size:100%;margin-bottom:0;list-style-type:inherit}.mw-parser-output .reflist-columns-2{column-width:30em}.mw-parser-output .reflist-columns-3{column-width:25em}.mw-parser-output .reflist-columns{margin-top:0.3em}.mw-parser-output .reflist-columns ol{margin-top:0}.mw-parser-output .reflist-columns li{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .reflist-upper-alpha{list-style-type:upper-alpha}.mw-parser-output .reflist-upper-roman{list-style-type:upper-roman}.mw-parser-output .reflist-lower-alpha{list-style-type:lower-alpha}.mw-parser-output .reflist-lower-greek{list-style-type:lower-greek}.mw-parser-output .reflist-lower-roman{list-style-type:lower-roman}</style><div class="reflist reflist-columns references-column-width reflist-columns-3"> <ol class="references"> <li id="cite_note-steinhardt-1"><span class="mw-cite-backlink">^ <a href="#cite_ref-steinhardt_1-0"><sup><i><b>a</b></i></sup></a> <a href="#cite_ref-steinhardt_1-1"><sup><i><b>b</b></i></sup></a> <a href="#cite_ref-steinhardt_1-2"><sup><i><b>c</b></i></sup></a> <a href="#cite_ref-steinhardt_1-3"><sup><i><b>d</b></i></sup></a></span> <span class="reference-text"><style data-mw-deduplicate="TemplateStyles:r1238218222">.mw-parser-output cite.citation{font-style:inherit;word-wrap:break-word}.mw-parser-output .citation q{quotes:"\"""\"""'""'"}.mw-parser-output .citation:target{background-color:rgba(0,127,255,0.133)}.mw-parser-output .id-lock-free.id-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/6/65/Lock-green.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-limited.id-lock-limited a,.mw-parser-output .id-lock-registration.id-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/d/d6/Lock-gray-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-subscription.id-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/a/aa/Lock-red-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .cs1-ws-icon a{background:url("//upload.wikimedia.org/wikipedia/commons/4/4c/Wikisource-logo.svg")right 0.1em center/12px no-repeat}body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-free a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-limited a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-registration a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-subscription a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .cs1-ws-icon a{background-size:contain;padding:0 1em 0 0}.mw-parser-output .cs1-code{color:inherit;background:inherit;border:none;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;color:var(--color-error,#d33)}.mw-parser-output .cs1-visible-error{color:var(--color-error,#d33)}.mw-parser-output .cs1-maint{display:none;color:#085;margin-left:0.3em}.mw-parser-output .cs1-kern-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right{padding-right:0.2em}.mw-parser-output .citation .mw-selflink{font-weight:inherit}@media screen{.mw-parser-output .cs1-format{font-size:95%}html.skin-theme-clientpref-night .mw-parser-output .cs1-maint{color:#18911f}}@media screen and (prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .cs1-maint{color:#18911f}}</style><cite id="CITEREFGibbonsHawkingSiklos1983" class="citation book cs1"><a href="/wiki/Gary_Gibbons" title="Gary Gibbons">Gibbons, Gary W.</a>; <a href="/wiki/Stephen_Hawking" title="Stephen Hawking">Hawking, Stephen W.</a>; Siklos, S.T.C., eds. (1983). "Natural Inflation". <i>The Very Early Universe</i>. <a href="/wiki/Cambridge_University_Press" title="Cambridge University Press">Cambridge University Press</a>. pp. 251–66. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-521-31677-4" title="Special:BookSources/978-0-521-31677-4"><bdi>978-0-521-31677-4</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=bookitem&rft.atitle=Natural+Inflation&rft.btitle=The+Very+Early+Universe&rft.pages=251-66&rft.pub=Cambridge+University+Press&rft.date=1983&rft.isbn=978-0-521-31677-4&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-vilenkin-2"><span class="mw-cite-backlink">^ <a href="#cite_ref-vilenkin_2-0"><sup><i><b>a</b></i></sup></a> <a href="#cite_ref-vilenkin_2-1"><sup><i><b>b</b></i></sup></a> <a href="#cite_ref-vilenkin_2-2"><sup><i><b>c</b></i></sup></a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFVilenkin1983" class="citation journal cs1">Vilenkin, Alexander (1983). "Birth of Inflationary Universes". <i>Physical Review D</i>. <b>27</b> (12): 2848–2855. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1983PhRvD..27.2848V">1983PhRvD..27.2848V</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1103%2FPhysRevD.27.2848">10.1103/PhysRevD.27.2848</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Physical+Review+D&rft.atitle=Birth+of+Inflationary+Universes&rft.volume=27&rft.issue=12&rft.pages=2848-2855&rft.date=1983&rft_id=info%3Adoi%2F10.1103%2FPhysRevD.27.2848&rft_id=info%3Abibcode%2F1983PhRvD..27.2848V&rft.aulast=Vilenkin&rft.aufirst=Alexander&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-eternal-3"><span class="mw-cite-backlink"><b><a href="#cite_ref-eternal_3-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGuth2007" class="citation journal cs1">Guth, Alan H. (2007). "Eternal inflation and its implications". <i>J. Phys. A</i>. <b>40</b> (25): 6811–6826. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/hep-th/0702178">hep-th/0702178</a></span>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2007JPhA...40.6811G">2007JPhA...40.6811G</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1088%2F1751-8113%2F40%2F25%2FS25">10.1088/1751-8113/40/25/S25</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:18669045">18669045</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=J.+Phys.+A&rft.atitle=Eternal+inflation+and+its+implications&rft.volume=40&rft.issue=25&rft.pages=6811-6826&rft.date=2007&rft_id=info%3Aarxiv%2Fhep-th%2F0702178&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A18669045%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1088%2F1751-8113%2F40%2F25%2FS25&rft_id=info%3Abibcode%2F2007JPhA...40.6811G&rft.aulast=Guth&rft.aufirst=Alan+H.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-4"><span class="mw-cite-backlink"><b><a href="#cite_ref-4">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGuth1981" class="citation journal cs1">Guth, Alan H. (1981). <a rel="nofollow" class="external text" href="https://doi.org/10.1103%2FPhysRevD.23.347">"Inflationary universe: A possible solution to the horizon and flatness problems"</a>. <i>Phys. Rev. D</i>. <b>23</b> (2): 347–356. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1981PhRvD..23..347G">1981PhRvD..23..347G</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://doi.org/10.1103%2FPhysRevD.23.347">10.1103/PhysRevD.23.347</a></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Phys.+Rev.+D&rft.atitle=Inflationary+universe%3A+A+possible+solution+to+the+horizon+and+flatness+problems&rft.volume=23&rft.issue=2&rft.pages=347-356&rft.date=1981&rft_id=info%3Adoi%2F10.1103%2FPhysRevD.23.347&rft_id=info%3Abibcode%2F1981PhRvD..23..347G&rft.aulast=Guth&rft.aufirst=Alan+H.&rft_id=https%3A%2F%2Fdoi.org%2F10.1103%252FPhysRevD.23.347&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-journals.aps.org-5"><span class="mw-cite-backlink"><b><a href="#cite_ref-journals.aps.org_5-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFAlbrechtSteinhardt1982" class="citation journal cs1">Albrecht, A.; Steinhardt, P. J. (1982). "Cosmology For Grand Unified Theories With Radiatively Induced Symmetry Breaking". <i>Phys. Rev. Lett</i>. <b>48</b> (17): 1220–1223. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1982PhRvL..48.1220A">1982PhRvL..48.1220A</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1103%2FPhysRevLett.48.1220">10.1103/PhysRevLett.48.1220</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Phys.+Rev.+Lett.&rft.atitle=Cosmology+For+Grand+Unified+Theories+With+Radiatively+Induced+Symmetry+Breaking&rft.volume=48&rft.issue=17&rft.pages=1220-1223&rft.date=1982&rft_id=info%3Adoi%2F10.1103%2FPhysRevLett.48.1220&rft_id=info%3Abibcode%2F1982PhRvL..48.1220A&rft.aulast=Albrecht&rft.aufirst=A.&rft.au=Steinhardt%2C+P.+J.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-6"><span class="mw-cite-backlink"><b><a href="#cite_ref-6">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFLinde,_A.D.1986" class="citation journal cs1">Linde, A.D. (August 1986). <a rel="nofollow" class="external text" href="http://www.stanford.edu/~alinde/Eternal86.pdf">"Eternally Existing Self-Reproducing Chaotic Inflationary Universe"</a> <span class="cs1-format">(PDF)</span>. <i>Physics Letters B</i>. <b>175</b> (4): 395–400. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1986PhLB..175..395L">1986PhLB..175..395L</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1016%2F0370-2693%2886%2990611-8">10.1016/0370-2693(86)90611-8</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Physics+Letters+B&rft.atitle=Eternally+Existing+Self-Reproducing+Chaotic+Inflationary+Universe&rft.volume=175&rft.issue=4&rft.pages=395-400&rft.date=1986-08&rft_id=info%3Adoi%2F10.1016%2F0370-2693%2886%2990611-8&rft_id=info%3Abibcode%2F1986PhLB..175..395L&rft.au=Linde%2C+A.D.&rft_id=http%3A%2F%2Fwww.stanford.edu%2F~alinde%2FEternal86.pdf&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-7"><span class="mw-cite-backlink"><b><a href="#cite_ref-7">^</a></b></span> <span class="reference-text">Linde, Andrei. "Inflationary cosmology." Inflationary cosmology. Springer Berlin Heidelberg, 2008. 1–54.</span> </li> <li id="cite_note-8"><span class="mw-cite-backlink"><b><a href="#cite_ref-8">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMukhanovChibisov1981" class="citation journal cs1">Mukhanov, ViatcheslavF.; Chibisov, G. V. (1981). "Quantum fluctuation and "nonsingular" universe". <i>JETP Letters</i>. <b>33</b>: 532–5. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1981JETPL..33..532M">1981JETPL..33..532M</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=JETP+Letters&rft.atitle=Quantum+fluctuation+and+%22nonsingular%22+universe&rft.volume=33&rft.pages=532-5&rft.date=1981&rft_id=info%3Abibcode%2F1981JETPL..33..532M&rft.aulast=Mukhanov&rft.aufirst=ViatcheslavF.&rft.au=Chibisov%2C+G.+V.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-9"><span class="mw-cite-backlink"><b><a href="#cite_ref-9">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMukhanov1982" class="citation journal cs1">Mukhanov, Viatcheslav F. (1982). "The vacuum energy and large scale structure of the universe". <i>Soviet Physics JETP</i>. <b>56</b> (2): 258–65. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1982JETP...56..258M">1982JETP...56..258M</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Soviet+Physics+JETP&rft.atitle=The+vacuum+energy+and+large+scale+structure+of+the+universe&rft.volume=56&rft.issue=2&rft.pages=258-65&rft.date=1982&rft_id=info%3Abibcode%2F1982JETP...56..258M&rft.aulast=Mukhanov&rft.aufirst=Viatcheslav+F.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-10"><span class="mw-cite-backlink"><b><a href="#cite_ref-10">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFStarobinsky,_A._A.1979" class="citation journal cs1">Starobinsky, A. A. (1979). <a rel="nofollow" class="external text" href="https://web.archive.org/web/20171215184314/http://www.jetpletters.ac.ru/ps/1370/article_20738.pdf">"Spectrum of Relict Gravitational Radiation and The Early State of the Universe"</a> <span class="cs1-format">(PDF)</span>. <i>JETP Lett</i>. <b>30</b>: 682. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1979JETPL..30..682S">1979JETPL..30..682S</a>. Archived from <a rel="nofollow" class="external text" href="http://www.jetpletters.ac.ru/ps/1370/article_20738.pdf">the original</a> <span class="cs1-format">(PDF)</span> on 15 December 2017<span class="reference-accessdate">. Retrieved <span class="nowrap">31 December</span> 2009</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=JETP+Lett.&rft.atitle=Spectrum+of+Relict+Gravitational+Radiation+and+The+Early+State+of+the+Universe&rft.volume=30&rft.pages=682&rft.date=1979&rft_id=info%3Abibcode%2F1979JETPL..30..682S&rft.au=Starobinsky%2C+A.+A.&rft_id=http%3A%2F%2Fwww.jetpletters.ac.ru%2Fps%2F1370%2Farticle_20738.pdf&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-11"><span class="mw-cite-backlink"><b><a href="#cite_ref-11">^</a></b></span> <span class="reference-text">See Guth (1997) for a popular description of the workshop, or <i>The Very Early Universe</i>, <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/0521316774" title="Special:BookSources/0521316774">0521316774</a> eds Hawking, Gibbon & Siklos for a more detailed report</span> </li> <li id="cite_note-12"><span class="mw-cite-backlink"><b><a href="#cite_ref-12">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHawking1982" class="citation journal cs1">Hawking, Stephen W. (1982). "The development of irregularities in a single bubble inflationary universe". <i>Physics Letters B</i>. <b>115</b> (4): 295–297. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1982PhLB..115..295H">1982PhLB..115..295H</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1016%2F0370-2693%2882%2990373-2">10.1016/0370-2693(82)90373-2</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Physics+Letters+B&rft.atitle=The+development+of+irregularities+in+a+single+bubble+inflationary+universe&rft.volume=115&rft.issue=4&rft.pages=295-297&rft.date=1982&rft_id=info%3Adoi%2F10.1016%2F0370-2693%2882%2990373-2&rft_id=info%3Abibcode%2F1982PhLB..115..295H&rft.aulast=Hawking&rft.aufirst=Stephen+W.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-13"><span class="mw-cite-backlink"><b><a href="#cite_ref-13">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFStarobinsky1982" class="citation journal cs1">Starobinsky, Alexei A. (1982). "Dynamics of phase transition in the new inflationary universe scenario and generation of perturbations". <i>Physics Letters B</i>. <b>117</b> (3–4): 175–8. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1982PhLB..117..175S">1982PhLB..117..175S</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1016%2F0370-2693%2882%2990541-X">10.1016/0370-2693(82)90541-X</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Physics+Letters+B&rft.atitle=Dynamics+of+phase+transition+in+the+new+inflationary+universe+scenario+and+generation+of+perturbations&rft.volume=117&rft.issue=3%E2%80%934&rft.pages=175-8&rft.date=1982&rft_id=info%3Adoi%2F10.1016%2F0370-2693%2882%2990541-X&rft_id=info%3Abibcode%2F1982PhLB..117..175S&rft.aulast=Starobinsky&rft.aufirst=Alexei+A.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AEternal+inflation" class="Z3988"></span></span> </li> <li id="cite_note-14"><span class="mw-cite-backlink"><b><a href="#cite_ref-14">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGuthPi1982" class="citation journal cs1">Guth, A.H.; <a href="/wiki/So-Young_Pi" title="So-Young Pi">Pi, So-Young</a> (1982). 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href="https://www.bbc.co.uk/news/science-environment-14372387">'Multiverse' theory suggested by microwave background</a>, BBC News, 3 August 2011 about testing eternal inflation.</li></ul> <div class="navbox-styles"><style data-mw-deduplicate="TemplateStyles:r1129693374">.mw-parser-output .hlist dl,.mw-parser-output .hlist ol,.mw-parser-output .hlist ul{margin:0;padding:0}.mw-parser-output .hlist dd,.mw-parser-output .hlist dt,.mw-parser-output .hlist li{margin:0;display:inline}.mw-parser-output .hlist.inline,.mw-parser-output .hlist.inline dl,.mw-parser-output .hlist.inline ol,.mw-parser-output .hlist.inline ul,.mw-parser-output .hlist dl dl,.mw-parser-output .hlist dl ol,.mw-parser-output .hlist dl ul,.mw-parser-output .hlist ol dl,.mw-parser-output .hlist ol ol,.mw-parser-output .hlist ol ul,.mw-parser-output .hlist ul dl,.mw-parser-output .hlist ul ol,.mw-parser-output .hlist ul ul{display:inline}.mw-parser-output .hlist .mw-empty-li{display:none}.mw-parser-output .hlist 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style="font-size:114%;margin:0 4em"><a href="/wiki/Quantum_gravity" title="Quantum gravity">Quantum gravity</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Central concepts</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/AdS/CFT_correspondence" title="AdS/CFT correspondence">AdS/CFT correspondence</a></li> <li><a href="/wiki/Batalin%E2%80%93Vilkovisky_formalism" title="Batalin–Vilkovisky formalism">Batalin–Vilkovisky formalism</a></li> <li><a href="/wiki/CA-duality" title="CA-duality">CA-duality</a></li> <li><a href="/wiki/Causal_patch" title="Causal patch">Causal patch</a></li> <li><a href="/wiki/Faddeev%E2%80%93Popov_ghost" title="Faddeev–Popov ghost">Faddeev–Popov ghost</a></li> <li><a href="/wiki/Gravitational_anomaly" title="Gravitational anomaly">Gravitational anomaly</a></li> <li><a href="/wiki/Graviton" title="Graviton">Graviton</a></li> <li><a href="/wiki/Holographic_principle" title="Holographic principle">Holographic principle</a></li> <li><a href="/wiki/IR/UV_mixing" title="IR/UV mixing">IR/UV mixing</a></li> <li><a href="/wiki/Planck_units" title="Planck units">Planck units</a></li> <li><a href="/wiki/Quantum_foam" title="Quantum foam">Quantum foam</a></li> <li><a href="/wiki/Ryu%E2%80%93Takayanagi_conjecture" title="Ryu–Takayanagi conjecture">Ryu–Takayanagi conjecture</a></li> <li><a href="/wiki/Trans-Planckian_problem" title="Trans-Planckian problem">Trans-Planckian problem</a></li> <li><a href="/wiki/Weinberg%E2%80%93Witten_theorem" title="Weinberg–Witten theorem">Weinberg–Witten theorem</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Toy_model" title="Toy model">Toy models</a></th><td class="navbox-list-with-group navbox-list navbox-even hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/(2%2B1)-dimensional_topological_gravity" title="(2+1)-dimensional topological gravity">2+1D topological gravity</a></li> <li><a href="/wiki/CGHS_model" title="CGHS model">CGHS model</a></li> <li><a href="/wiki/Jackiw%E2%80%93Teitelboim_gravity" title="Jackiw–Teitelboim gravity">Jackiw–Teitelboim gravity</a></li> <li><a href="/wiki/Liouville_gravity" class="mw-redirect" title="Liouville gravity">Liouville gravity</a></li> <li><a href="/wiki/RST_model" title="RST model">RST model</a></li> <li><a href="/wiki/Topological_quantum_field_theory" title="Topological quantum field theory">Topological quantum field theory</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Quantum_field_theory_in_curved_spacetime" title="Quantum field theory in curved spacetime">Quantum field theory<br />in curved spacetime</a></th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Bunch%E2%80%93Davies_vacuum" title="Bunch–Davies vacuum">Bunch–Davies vacuum</a></li> <li><a href="/wiki/Hawking_radiation" title="Hawking radiation">Hawking radiation</a></li> <li><a href="/wiki/Semiclassical_gravity" title="Semiclassical gravity">Semiclassical gravity</a></li> <li><a href="/wiki/Unruh_effect" title="Unruh effect">Unruh effect</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Black_hole" title="Black hole">Black holes</a></th><td class="navbox-list-with-group navbox-list navbox-even hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Black_hole_complementarity" title="Black hole complementarity">Black hole complementarity</a></li> <li><a href="/wiki/Black_hole_information_paradox" title="Black hole information paradox">Black hole information paradox</a></li> <li><a href="/wiki/Black_hole_thermodynamics" title="Black hole thermodynamics">Black-hole thermodynamics</a></li> <li><a href="/wiki/Bekenstein_bound" title="Bekenstein bound">Bekenstein bound</a></li> <li><a href="/wiki/Bousso%27s_holographic_bound" title="Bousso's holographic bound">Bousso's holographic bound</a></li> <li><a href="/wiki/Cosmic_censorship_hypothesis" title="Cosmic censorship hypothesis">Cosmic censorship hypothesis</a></li> <li><a href="/wiki/ER_%3D_EPR" title="ER = EPR">ER = EPR</a></li> <li><a href="/wiki/Firewall_(physics)" title="Firewall (physics)">Firewall (physics)</a></li> <li><a href="/wiki/Gravitational_singularity" title="Gravitational singularity">Gravitational singularity</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Approaches</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/String_theory" title="String theory">String theory</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Bosonic_string_theory" title="Bosonic string theory">Bosonic string theory</a></li> <li><a href="/wiki/M-theory" title="M-theory">M-theory</a></li> <li><a href="/wiki/Supergravity" title="Supergravity">Supergravity</a></li> <li><a href="/wiki/Superstring_theory" title="Superstring theory">Superstring theory</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Canonical_quantum_gravity" title="Canonical quantum gravity">Canonical quantum gravity</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Loop_quantum_gravity" title="Loop quantum gravity">Loop quantum gravity</a></li> <li><a href="/wiki/Wheeler%E2%80%93DeWitt_equation" title="Wheeler–DeWitt equation">Wheeler–DeWitt equation</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Euclidean_quantum_gravity" title="Euclidean quantum gravity">Euclidean quantum gravity</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Hartle%E2%80%93Hawking_state" title="Hartle–Hawking state">Hartle–Hawking state</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Others</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Causal_dynamical_triangulation" title="Causal dynamical triangulation">Causal dynamical triangulation</a></li> <li><a href="/wiki/Causal_sets" title="Causal sets">Causal sets</a></li> <li><a href="/wiki/Dual_graviton" title="Dual graviton">Dual graviton</a></li> <li><a href="/wiki/Group_field_theory" title="Group field theory">Group field theory</a></li> <li><a href="/wiki/Noncommutative_geometry" title="Noncommutative geometry">Noncommutative geometry</a></li> <li><a href="/wiki/Spin_foam" title="Spin foam">Spin foam</a></li> <li><a href="/wiki/Superfluid_vacuum_theory" title="Superfluid vacuum theory">Superfluid vacuum theory</a></li> <li><a href="/wiki/Twistor_theory" title="Twistor theory">Twistor theory</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Applications</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Quantum_cosmology" title="Quantum cosmology">Quantum cosmology</a> <ul><li><a class="mw-selflink selflink">Eternal inflation</a></li> <li><a href="/wiki/FRW/CFT_duality" title="FRW/CFT duality">FRW/CFT duality</a></li> <li><a href="/wiki/Multiverse" title="Multiverse">Multiverse</a></li></ul></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="2"><div><i>See also:</i> <span class="noviewer" typeof="mw:File"><span title="Template"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Symbol_template_class_pink.svg/16px-Symbol_template_class_pink.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Symbol_template_class_pink.svg/23px-Symbol_template_class_pink.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/83/Symbol_template_class_pink.svg/31px-Symbol_template_class_pink.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Template:Quantum_mechanics_topics" title="Template:Quantum mechanics topics">Template:Quantum mechanics topics</a></div></td></tr></tbody></table></div>    </div><noscript><img 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