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Scalar correlation functions for a double-well potential in de Sitter

Thus, S p n + p ( c) is an ( n + p) - dimensional indefinite Riemannian manifold of index p and of constant curvature c . It is called an ( n + p) - dimensional de Sitter space of constant curvature c and of index p . E. This is referred to as a slicing of the space, and it is, actually, possible to slice the space in three different ways that correspond to cosmologically expanding spaces with flat, positively-curved and negatively curved spatial parts, respectively. These are the ways of describing de Sitter space that are useful when considering inflation. A de Sitter universe is a cosmological solution to the Einstein field equations of general relativity, named after Willem de Sitter. It models the universe as spatially flat and neglects ordinary matter, so the dynamics of the universe are dominated by the cosmological constant , thought to correspond to dark energy in our universe or the inflaton field in the early universe . The Herschel Space Observatory is a European Space Agency space observatory sensitive to the far infrared and submillimetre wavebands.

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Your interpretation is right, but it's important to notice that time as defined here (the one in which the spatial 3-sphere contracts and expands) isn't a Killing vector of the spacetime, i.e. isn't a symmetry like in Minkowski space. A de Sitter universe is a cosmological solution to the Einstein field equations of general relativity, named after Willem de Sitter.It models the universe as spatially flat and neglects ordinary matter, so the dynamics of the universe are dominated by the cosmological constant, thought to correspond to dark energy in our universe or the inflaton field in the early universe. 2021-03-17 "De Sitter's space-time is an exact solution of the equations of ordinary general relativity discovered as early as 1917, empty of matter but which includes a repulsive force called the 2004-03-01 de Sitter space, we will see that this property is not true by answering the question: can any two points which are connected through a timelike curve also be connected through a timelike geodesic? A related question can be asked for De Sitter spacelike curves and geodesics. IV. 2021-02-12 What does de-sitter-space mean?

## FLUX THEORY - Dissertations.se

Our universe seems to be asymptotically de Sitter at very early and very late times: At redshifts of ~0.5 and later (late times being low redshift and the future), the universe seems to be dominated by dark energy (see What is dark energy? Why does it matter? metric of constant curvature. This is known as de Sitter space dSn.

### Road to Emergent Spacetime

complete space-like submanifolds in a. Let R p n + p + 1 be an ( n + p + 1) - dimensional Minkowski space of index p , i.e., R p n + p + 1 = { ( x 1 … x n + p + 1) ∈ R n + p + 1 } and is equipped with the Lorentz metric ∑ i = 1 n + 1 ( d x i) 2 − ∑ j = 1 p ( d x n + 1 + j) 2 . A standard topic in an introductory General Relativity (GR) course is the study of maximally symmetric solutions. These are flat (Minkowski) spacetime, de Sitter spacetime (obtained when the cosmological constant is positive) and Anti-de Sitter spacetime (when the cosmological constant is negative).

metric space with positive curvature R>0 called de Sit-ter Space (abbreviated dS), and the space with negative curvature R<0 called Anti-de Sitter space (abbreviated AdS). II. (ANTI-)DE SITTER SPACE-TIMES A simple way to understand the n-dimensional De Sitter space (dS n) is by its embedding in a (n+1)-dimensional at space Rn;1 with Cartesian coordinates
2001-09-30 · These lectures present an elementary discussion of some background material relevant to the problem of de Sitter quantum gravity. The first two lectures discuss the classical geometry of de Sitter space and properties of quantum field theory on de Sitter space, especially the temperature and entropy of de Sitter space. The final lecture contains a pedagogical discussion of the appearance of
230 B Allen / Phase transltlons tn De Sitter space Each observer in De Sitter space has an event horizon, which he observes radiating a thermal spectrum of particles [5], at a temperature H/2rr. This is the lowest equilibrium temperature that any matter can have.

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1032s,isapproximatelyde Sitter spacetime. We will now take a detour to apply our methods to de Sitter space, since in this situation they produce observable e↵ects via the imprint of primordial density perturbations on the CMB. de Der De-Sitter-Raum wurde 1917 von Willem de Sitter entdeckt und gleichzeitig – unabhängig von de Sitter – von Tullio Levi-Civita. en De Sitter space can be defined as a submanifold of a generalized Minkowski space of one higher dimension. Willem de Sitter, född den 6 maj 1872, död den 20 november 1934, var en namnkunnig matematiker, astronom och kosmolog i Nederländerna.Han blev mest uppmärksammad för sina bidrag till utvecklingen av den fysikaliska kosmologin.

Willem de Sitter and Albert Einstein worked together closely in Leiden in the 1920s on the spacetime structure of the universe. Manifolds of constant curvature are most familiar
2020-06-05 · S p n + p ( c) = { x ∈ R p n + p + 1: x 1 2 + ⋯ + x n + 1 2 − x n + 2 2 − ⋯ − x n + p + 1 2 = 1 / c }. Thus, S p n + p ( c) is an ( n + p) - dimensional indefinite Riemannian manifold of index p and of constant curvature c . It is called an ( n + p) - dimensional de Sitter space of constant curvature c and of index p . E.
This is referred to as a slicing of the space, and it is, actually, possible to slice the space in three different ways that correspond to cosmologically expanding spaces with flat, positively-curved and negatively curved spatial parts, respectively. These are the ways of describing de Sitter space that are useful when considering inflation.

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Physical Review D, 2002. Andrei Linde searching for De Sitter space 27 found (95 total) alternate case: de Sitter space. Steven Gubser (577 words) case mismatch in snippet view article find links to article and is commonly known, along with Edward Witten's 1998 work Anti De Sitter Space And Holography, as the GKPW dictionary. De Sitter space can also be defined as the quotient O(1, n) / O(1, n − 1) of two indefinite orthogonal groups, which shows that it is a non-Riemannian symmetric space. Topologically, de Sitter space is R × S n−1 (so that if n ≥ 3 then de Sitter space is simply connected).

as Schwarzschild black holes in asymptotically anti-de Sitter (AdS) space, it is often di cult to say what it means to be behind the horizon in the dual theory. A possible alternative approach is to consider string theory in the near horizon geometry of a black hole. The latter takes the form AdS 2 S2 for extremal black holes in four dimensions. The Herschel Space Observatory is a European Space Agency space observatory sensitive to the far infrared and submillimetre wavebands. The Herschel Observatory is capable of seeing the coldest and dustiest objects in space; for example, cool cocoons where stars form and dusty galaxies just starting to bulk up with new stars. [via NASA/JPL]
We discuss how the S-matrix formulation of quantum gravity eliminates de Sitter vacua, both stable or meta-stable. The S-matrix constraint is enforced by the phenomenon of anomalous quantum break-time.

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to a de Sitter (dS) spacetime in the inﬁnite future (I+). Interestingly, the proper char-acterization of dynamics in such asymptotically future dS spacetimes - the analog of the S-matrix for asymptotically Minkowski spacetimes or boundary correlators for asymp-totically anti-de Sitter (AdS) spacetimes - remains an open problem. In this paper we Conformal scattering of the Maxwell-scalar eld system on de Sitter space Grigalius Taujanskas∗ Mathematical Institute Oxford University Radcliffe Observatory Quarter Oxford OX2 dimensional de Sitter space, which leads to the dS/CFT correspondence [27]. This section also contains a derivation, missing in previous treatments, of the. De-sitter space is a mathematical construct, it gives a starting point to give coordinates in space/time. First look into how coordinates actually work, there is a Dec 6, 2019 As a consequence of the accelerated expansion, an inertial observer in de Sitter ( dS) space is causally connected with only a subregion of the full A USEFUL FORM OF THE DE SITTER METRIC. We define a locally spherically symmetric three-space as a space that can be covered with charts in which the May 28, 2020 We consider small perturbations to a static three-dimensional de Sitter geometry.