advanced_tools:group_theory:desitter

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advanced_tools:group_theory:desitter [2018/03/24 11:05] jakobadmin [Layman] |
advanced_tools:group_theory:desitter [2018/03/24 11:10] (current) jakobadmin [FAQ] |
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<tabbox Why is it interesting?> | <tabbox Why is it interesting?> | ||

+ | The simple existence of a non-vanishing cosmological constant in the universe means that the [[advanced_tools:group_theory:poincare_group|Poincare group]] is no longer the kinematic group of spacetime; this is a largely overlooked point. | ||

+ | |||

+ | The present experimental value for the cosmological constant is tiny but nonzero: $\Lambda \approx 1.19·10^{−52}$ $1/m^2$. | ||

+ | |||

+ | The Poincare group is the contraction of the deSitter group in the limit $\Lambda \rightarrow 0$, analogous to how the Galilean group is the contraction of the Poincare group in the limit $c\rightarrow \infty$. | ||

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+ | Thus a non-zero $\Lambda$ means that the exact spacetime symmetry group is the deSitter group and the Poincare group is only a good approximation because $\Lambda$ is so small. | ||

+ | |||

+ | C.f. http://physics.stackexchange.com/questions/299621/the-desitter-group-vs-the-poincare-group-for-a-non-zero-cosmological-constant | ||

+ | |||

+ | ---- | ||

<blockquote>Given the current picture of an increasingly expanding universe, it may very well be the case that future generations of students first learn about the de Sitter and the Newton-Hooke groups, while the Poincaré and the Galilei groups will be considered to be nothing but historical aberrations. <cite>Symmetries in Fundamental Physics by Kurt Sundermeyer</cite></blockquote> | <blockquote>Given the current picture of an increasingly expanding universe, it may very well be the case that future generations of students first learn about the de Sitter and the Newton-Hooke groups, while the Poincaré and the Galilei groups will be considered to be nothing but historical aberrations. <cite>Symmetries in Fundamental Physics by Kurt Sundermeyer</cite></blockquote> | ||

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+ | |||

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+ | <blockquote> | ||

+ | Since the renormalized value of the cosmological constant is experimentally quite small, $ρ ∼ 10^{−122}M_{Pl} \sim 10^{−3}$ eV (and positive – **we live in de Sitter space**), we can ignore it for terrestrial experiments. To account for a non- zero cosmological constant in quantum field theory requires field theory in curved space, a topic beyond the scope of this text. | ||

+ | |||

+ | <cite>Page 415 in Schwartz - Quantum Field Theory and the Standard Model</cite> | ||

+ | </blockquote> | ||

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+ | |||

+ | |||

+ | <blockquote> | ||

+ | To the extent that* ~$74 \simeq 100$ %, we can say that our universe is observed to be almost maximally symmetric and de Sitter.(*Dark energy amounts to ~74% of the universe [...]). | ||

+ | [..] | ||

+ | Our universe might very well be described by $dS^4$ to a good approximation, as discussed in chapter VIII.2 and in the preceding section. | ||

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+ | <cite>Einstein Gravity in a Nutshell - A. Zee</cite> | ||

+ | </blockquote> | ||

+ | |||

+ | |||

+ | <blockquote> | ||

+ | We will confront certain recent astronomical observations suggesting that, even in an empty universe, the event | ||

+ | world may possess properties not reflected in the structure of Minkowski | ||

+ | spacetime, at least on the cosmological scale. Remarkably, there is a viable | ||

+ | alternative [the deSitter spacetime], nearly 100 years old, that has precisely these properties and we | ||

+ | will devote a little time to becoming acquainted with it. | ||

+ | |||

+ | <cite>The Geometry of Minkowski Spacetime - Naber</cite> | ||

+ | </blockquote> | ||

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+ | In addition: | ||

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+ | <blockquote>"Apart from the current accelerating cosmic expansion, further motivation for the interest | ||

+ | in de Sitter gravity comes from the inflationary era, during which one assumes that the | ||

+ | universe was also described by a de Sitter phase." [[https://arxiv.org/pdf/hep-th/0407255.pdf|Aspects of Quantum Gravity in de Sitter Spaces Dietmar Klemm and Luciano Vanzo]]</blockquote> | ||

+ | |||

+ | <blockquote>In quantum field theory (in its present imperfect form) the Minkowski metric is the vacuum expectation value of the Riemannian metric. It seems unsafe to restrict the attention arbitrarily to the special case of vanishing cosmological constant, for this ease is unstable to deformations; a nonzero cosmological constant may, for example, appear spontaneously through renormalization. In that case the zeroth approximation (or vacuum expectation value) of the metric cannot be Minkowski, but must be de Sitter. Our previous analysis must therefore be modified by the substitution of the de Sitter group for the Poincare group | ||

+ | <cite> from [[http://journals.aps.org/prd/pdf/10.1103/PhysRevD.23.1278|Massless particles, conformal group, and de Sitter Universe by E. Angelopoulos]] </cite></blockquote> | ||

+ | |||

+ | General relativity can be formulated as a gauge theory of the deSitter group, see http://journals.aps.org/prd/pdf/10.1103/PhysRevD.21.1466. | ||

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<tabbox Layman> | <tabbox Layman> | ||

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The deSitter group becomes the Poincare group in the contraction limit $R \rightarrow \infty$, where $R$ is the so-called deSitter radius. Oftentimes, people prefer to work with the [[open_problems:cosmological_constant|cosmological constant]] $ \Lambda \propto \frac{1}{R^2}$ instead. Analogously, the Poincare group becomes the Galilean group in the $c \rightarrow \infty$ limit. | The deSitter group becomes the Poincare group in the contraction limit $R \rightarrow \infty$, where $R$ is the so-called deSitter radius. Oftentimes, people prefer to work with the [[open_problems:cosmological_constant|cosmological constant]] $ \Lambda \propto \frac{1}{R^2}$ instead. Analogously, the Poincare group becomes the Galilean group in the $c \rightarrow \infty$ limit. | ||

+ | |||

+ | The fact that the deSitter group contracts to the Poincare group in the $R\rightarrow \infty$ limit, means that the Poincare group is a good approximation as long as we consider systems with a length scale that is small compared to $R$. This is analogous to how the Galilean group is good enough as long as we are only dealing with velocities much smaller than the invariant velocity $c$. | ||

+ | |||

+ | Expressed differently: the deSitter group is only important for cosmological systems, which have a length scale comparable to $R$. | ||

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+ | Alternatively, we can talk about the invariant energy scale $\Lambda$. The deSitter group contracts to the Poincare group in the $\Lambda \rightarrow 0$ limit. Thus the deSitter structure is not important, as long as we are dealing with energies much larger than $\Lambda$. In systems with energies much larger than $\Lambda$ such a small constant energy has no effect. The present day value for the cosmological constant is $\Lambda \approx 10^{-56} \mathrm{m^{-2}}$ and this means that present day effects of the deSitter group structure are tiny. This means, the Poincare group is a great approximate symmetry nowadays, because $\Lambda$ is almost zero. | ||

+ | |||

+ | However, the deSitter group could be very important in the early universe, too. For example, because it seems plausible that there was [[https://en.wikipedia.org/wiki/Inflation_(cosmology)|a phase when the cosmological constant was much higher]]. | ||

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<tabbox Student> | <tabbox Student> | ||

- | <note tip> | + | <blockquote> |

- | In this section things should be explained by analogy and with pictures and, if necessary, some formulas. | + | The group $SO(d,1)$ moves points on $dS^d$ around. We thus conclude that, just like the sphere, deSitter spacetime is maximally symmetric. So, according to the general theory of maximally symmetric spaces explained in chapter IX.6, the Riemann curvature tensor $R_{\mu\nu\lambda\sigma}$ must be equal to $(g_{\mu\lambda}g_{\nu\sigma}-g_{\mu\sigma}g_{\nu\lambda})$ up to an overall constant. [...] Then, by dimensional analysis, we must have |

- | </note> | + | $$ R_{\mu\nu\lambda\sigma} =\frac{1}{L} (g_{\mu\lambda}g_{\nu\sigma}-g_{\mu\sigma}g_{\nu\lambda}) $$ |

+ | [...] de Sitter spacetime is a solution of Einstein's field equation $R_{\mu \nu}=8\pi G\Lambda g_{\mu\nu}$, with a positive cosmological constant given by | ||

+ | $$ 8\pi G\Lambda = \frac{3}{L}$$ | ||

+ | [...] | ||

+ | Topologically, de Sitter spacetime is $R \times S^3$, with a spatial section given by $S^3$, as just explained. In contrast, we know from chapters VI.2 and VI.5 that Einstein's field equation with a positive cosmological constant leads to $ds^2=-dt^2+e^{2Ht}(dx^2+dy^2+dz^2)$ with the Hubble constant given by $H= \left( \frac{8\pi G}{3}\Lambda\right)^{1/3}$, or in terms of the de Sitter length, $H=1/L$. | ||

+ | | ||

+ | <cite>page 627 in Einstein Gravity in a Nutshell - A. Zee</cite> | ||

+ | </blockquote> | ||

<tabbox Researcher> | <tabbox Researcher> | ||

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</note> | </note> | ||

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- | <tabbox Examples> | ||

- | --> Example1# | ||

- | | + | <tabbox FAQ> |

- | <-- | + | |

- | --> Example2:# | + | -->It ist confusing what a "five-dimensional" group like $SO(4,1)$ has to say about our four-dimensional world. Does this mean deSitter theories predict a fifth dimension?# |

+ | | ||

+ | No, recall that an explicit representation of the Poincare group is given by $(5 \times 5)$ matrices, too! This is, because the Lorentz group transformations are $(4 \times 4)$ matrices themselves and in oredr to describe translations, we need to make these matrices into $(5 \times 5)$ matrices. See, for example, chapter 4 "The Poincaré transformations" in [[http://www.springer.com/us/book/9783642154812|Symmetries and Group Theory in Particle Physics]] by Costa and Fogly. | ||

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<-- | <-- | ||

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- | <tabbox FAQ> | ||

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<tabbox History> | <tabbox History> |

advanced_tools/group_theory/desitter.1521885913.txt.gz · Last modified: 2018/03/24 10:05 (external edit)

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